subject:(Stars Rotation)

Columbia University

1. Nunez, Alejandro. The Relationship Between Stellar Rotation and Magnetic Activity as Revealed by M37 and Alpha Persei.

Degree: 2018, Columbia University

URL: https://doi.org/10.7916/D8V712F7

► In low-mass (≲1.2 M⊙) main-sequence stars, the combination of differential rotation and turbulent flows in the outer convective region generates strong magnetic fields. It has… (more)

Subjects/Keywords: Stars – Rotation; Stars – Magnetic fields; Low mass stars

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APA (6^th Edition):

Nunez, A. (2018). The Relationship Between Stellar Rotation and Magnetic Activity as Revealed by M37 and Alpha Persei. (Doctoral Dissertation). Columbia University. Retrieved from https://doi.org/10.7916/D8V712F7

Chicago Manual of Style (16^th Edition):

Nunez, Alejandro. “The Relationship Between Stellar Rotation and Magnetic Activity as Revealed by M37 and Alpha Persei.” 2018. Doctoral Dissertation, Columbia University. Accessed March 07, 2021. https://doi.org/10.7916/D8V712F7.

MLA Handbook (7^th Edition):

Nunez, Alejandro. “The Relationship Between Stellar Rotation and Magnetic Activity as Revealed by M37 and Alpha Persei.” 2018. Web. 07 Mar 2021.

Vancouver:

Nunez A. The Relationship Between Stellar Rotation and Magnetic Activity as Revealed by M37 and Alpha Persei. [Internet] [Doctoral dissertation]. Columbia University; 2018. [cited 2021 Mar 07]. Available from: https://doi.org/10.7916/D8V712F7.

Council of Science Editors:

Nunez A. The Relationship Between Stellar Rotation and Magnetic Activity as Revealed by M37 and Alpha Persei. [Doctoral Dissertation]. Columbia University; 2018. Available from: https://doi.org/10.7916/D8V712F7

Vanderbilt University

2. Le Blanc, Thompson S. The Role of Disks in the Angular Momentum Evolution of Young, Low-Mass Stars.

Degree: PhD, Physics, 2012, Vanderbilt University

URL: http://hdl.handle.net/1803/13325

► Detailed studies of the spectral energy distributions (SEDs) of young stars can reveal much about their basic properties and their circumstellar material. Previous work suggests… (more)

▼ Detailed studies of the spectral energy distributions (SEDs) of young stars can reveal much about their basic properties and their circumstellar material. Previous work suggests that the magnetic interactions of its circumstellar disk may be the result of the influence of a young stars angular momentum content and rotation rate. The generic prediction of these “disk-locking” theories is that a disk-locked star will be forced to rotate at the same Keplerian angular velocity of the inner edge of the disk; that is, the disks radius at which it is truncated or evacuated, should be equal to its co-rotation radius. Additional interpretations of these theories also suggest a correlation between the rotation period of a star and the structure of its circumstellar disk; slow rotators possess closely truncated disks that enforce the stars slow rotation, whereas rapid rotators possess disks that are largely evacuated or anemic, interpreted as being outside of the magnetic influence of the star, whereby the star is free to speed up as it continues its pre-main sequence contraction. As a test of the expectations of these theories, we model the spectral energy distributions of 33 young stars in the IC348 region with known rotation periods, as well as infrared excesses indicative of circumstellar disks. We match the observed SED for each star, sampling a range of 0.6-8.0m, to a grid of 200,000 pre-computed star+disk radiative transfer models, from which we then infer the circumstellar disks inner truncation radius. We then compare the inferred truncation radius to the disks co-rotation radius, calculated from the stars measured rotation period. We do not find any obvious differences in the disk truncation radii of slow versus rapid rotators. This holds true both at the level of whether close-in disk material is present at all, as well as analyzing the precise location of the inner edge of the disk relative to the co-rotation radius among the subset of stars with close-in disk material. One interpretation of these results is that the disk locking is unimportant for the IC 348 stars in our sample. Alternatively, if disk locking does operate, then it must operate on both slow and rapid rotators, potentially producing both spin-up and spin-down torques, and the transition from the disk-locked state to the disk-released state must occur more rapidly than the stellar contraction timescale. Advisors/Committee Members: Dr. David A. Weintraub (committee member), Dr. Andreas Berlind (committee member), Dr. David Ersnt (committee member), Dr. Antonella Nota (committee member), Dr. Keivan G. Stassun (Committee Chair).

Subjects/Keywords: circumstellar material; pre-main sequence; stars; rotation

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APA (6^th Edition):

Le Blanc, T. S. (2012). The Role of Disks in the Angular Momentum Evolution of Young, Low-Mass Stars. (Doctoral Dissertation). Vanderbilt University. Retrieved from http://hdl.handle.net/1803/13325

Chicago Manual of Style (16^th Edition):

Le Blanc, Thompson S. “The Role of Disks in the Angular Momentum Evolution of Young, Low-Mass Stars.” 2012. Doctoral Dissertation, Vanderbilt University. Accessed March 07, 2021. http://hdl.handle.net/1803/13325.

MLA Handbook (7^th Edition):

Le Blanc, Thompson S. “The Role of Disks in the Angular Momentum Evolution of Young, Low-Mass Stars.” 2012. Web. 07 Mar 2021.

Vancouver:

Le Blanc TS. The Role of Disks in the Angular Momentum Evolution of Young, Low-Mass Stars. [Internet] [Doctoral dissertation]. Vanderbilt University; 2012. [cited 2021 Mar 07]. Available from: http://hdl.handle.net/1803/13325.

Council of Science Editors:

Le Blanc TS. The Role of Disks in the Angular Momentum Evolution of Young, Low-Mass Stars. [Doctoral Dissertation]. Vanderbilt University; 2012. Available from: http://hdl.handle.net/1803/13325

Iowa State University

3. Bolie, Victor Wayne. Periodic orbits in the neighborhood of libration points in certain rotating systems.

Degree: 1952, Iowa State University

URL: https://lib.dr.iastate.edu/rtd/12905

Subjects/Keywords: Stars – Rotation; Mathematics

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APA (6^th Edition):

Bolie, V. W. (1952). Periodic orbits in the neighborhood of libration points in certain rotating systems. (Thesis). Iowa State University. Retrieved from https://lib.dr.iastate.edu/rtd/12905

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

Chicago Manual of Style (16^th Edition):

Bolie, Victor Wayne. “Periodic orbits in the neighborhood of libration points in certain rotating systems.” 1952. Thesis, Iowa State University. Accessed March 07, 2021. https://lib.dr.iastate.edu/rtd/12905.

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

MLA Handbook (7^th Edition):

Bolie, Victor Wayne. “Periodic orbits in the neighborhood of libration points in certain rotating systems.” 1952. Web. 07 Mar 2021.

Vancouver:

Bolie VW. Periodic orbits in the neighborhood of libration points in certain rotating systems. [Internet] [Thesis]. Iowa State University; 1952. [cited 2021 Mar 07]. Available from: https://lib.dr.iastate.edu/rtd/12905.

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

Council of Science Editors:

Bolie VW. Periodic orbits in the neighborhood of libration points in certain rotating systems. [Thesis]. Iowa State University; 1952. Available from: https://lib.dr.iastate.edu/rtd/12905

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

University of British Columbia

4. Woods, David. Luminosity - velocity diagrams of virgo cluster spiral galaxies.

Degree: MS- MSc, Geophysics, 1990, University of British Columbia

URL: http://hdl.handle.net/2429/29342

► Luminosity-velocity diagrams for 12 spiral galaxies in the Virgo cluster are presented. Optical rotation curves obtained for the innermost portions of eight galaxies, complemented with… (more)

Subjects/Keywords: Stars – Luminosity function; Stars – Rotation

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APA (6^th Edition):

Woods, D. (1990). Luminosity - velocity diagrams of virgo cluster spiral galaxies. (Masters Thesis). University of British Columbia. Retrieved from http://hdl.handle.net/2429/29342

Chicago Manual of Style (16^th Edition):

Woods, David. “Luminosity - velocity diagrams of virgo cluster spiral galaxies.” 1990. Masters Thesis, University of British Columbia. Accessed March 07, 2021. http://hdl.handle.net/2429/29342.

MLA Handbook (7^th Edition):

Woods, David. “Luminosity - velocity diagrams of virgo cluster spiral galaxies.” 1990. Web. 07 Mar 2021.

Vancouver:

Woods D. Luminosity - velocity diagrams of virgo cluster spiral galaxies. [Internet] [Masters thesis]. University of British Columbia; 1990. [cited 2021 Mar 07]. Available from: http://hdl.handle.net/2429/29342.

Council of Science Editors:

Woods D. Luminosity - velocity diagrams of virgo cluster spiral galaxies. [Masters Thesis]. University of British Columbia; 1990. Available from: http://hdl.handle.net/2429/29342

The Ohio State University

5. Sonneborn, George. A stability analysis of the equatorial regions of rapidly rotating B stars.

Degree: PhD, Graduate School, 1980, The Ohio State University

URL: http://rave.ohiolink.edu/etdc/view?acc_num=osu148715118016362

Subjects/Keywords: Physics; B stars; Stars – Rotation

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APA · Chicago · MLA · Vancouver · CSE | Export to Zotero / EndNote / Reference Manager

APA (6^th Edition):

Sonneborn, G. (1980). A stability analysis of the equatorial regions of rapidly rotating B stars. (Doctoral Dissertation). The Ohio State University. Retrieved from http://rave.ohiolink.edu/etdc/view?acc_num=osu148715118016362

Chicago Manual of Style (16^th Edition):

Sonneborn, George. “A stability analysis of the equatorial regions of rapidly rotating B stars.” 1980. Doctoral Dissertation, The Ohio State University. Accessed March 07, 2021. http://rave.ohiolink.edu/etdc/view?acc_num=osu148715118016362.

MLA Handbook (7^th Edition):

Sonneborn, George. “A stability analysis of the equatorial regions of rapidly rotating B stars.” 1980. Web. 07 Mar 2021.

Vancouver:

Sonneborn G. A stability analysis of the equatorial regions of rapidly rotating B stars. [Internet] [Doctoral dissertation]. The Ohio State University; 1980. [cited 2021 Mar 07]. Available from: http://rave.ohiolink.edu/etdc/view?acc_num=osu148715118016362.

Council of Science Editors:

Sonneborn G. A stability analysis of the equatorial regions of rapidly rotating B stars. [Doctoral Dissertation]. The Ohio State University; 1980. Available from: http://rave.ohiolink.edu/etdc/view?acc_num=osu148715118016362

6. Ahmed, Ahmed. Nitrogen Abundances in Early-Type Be Stars.

Degree: 2015, University of Western Ontario

URL: https://ir.lib.uwo.ca/etd/3354

► A sample of 26 Be stars from the Magnetism in Massive Stars (MiMeS) spectroscopic survey are analyzed for their photospheric nitrogen abundances in an effort… (more)

▼ A sample of 26 Be stars from the Magnetism in Massive Stars (MiMeS) spectroscopic survey are analyzed for their photospheric nitrogen abundances in an effort to detect rotational mixing in the Be stars. Be stars are massive stars, between 3 and 20 times the mass of the Sun, that are surrounded by a thin, equatorial disk of gas that produces emission lines in their optical and near-infrared spectra. Be stars are the most rapidly-rotating stellar population on the main sequence, where stars produce energy by core hydrogen burning. New, non-LTE line transfer calculations are performed for the Nii ion, the dominant ionization stage in the photospheres of the B stars, and an extensive error analysis is performed via Monte Carlo simulation to determine the achievable accuracy of nitrogen abundances among these stars. To analyze the measured Nii equivalent widths from the MiMeS survey, the effects of both gravitational darkening, due to the rapid rotation of the central B star, and the veiling effect of emission from the Be star circumstellar disk are considered. Both of these effects are found to be small for the sample population, affecting the final nitrogen abundances at the level ≈ ±0.1 dex. The final, average nitrogen abundance for the MiMeS sample, AMiMeS, N = 7.78, has a value in good agreement with the solar abundance, AN = 7.83, and recent, high-precision abundance measurements for main-sequence B stars. Nevertheless, the MiMeS sample standard deviation is over a factor of two larger than that of the observed nitrogen abundances in the atmospheres of B stars in the solar neighbourhood, with many low abundance objects and a few high abundance objects. No discernible trend of the nitrogen abundance can be seen with stellar gravity, log g (as a proxy for stellar age), or stellar equatorial velocity in the MiMeS survey. It is suggested that possible disk emission in the NII line transitions may explain the lower abundance objects, and this will be the subject of future work.

Subjects/Keywords: stars: abundances - stars: atmospheres -stars: rotation - radiative transfer -line: formation; Stars, Interstellar Medium and the Galaxy

11 more images…

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APA (6^th Edition):

Ahmed, A. (2015). Nitrogen Abundances in Early-Type Be Stars. (Thesis). University of Western Ontario. Retrieved from https://ir.lib.uwo.ca/etd/3354

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

Chicago Manual of Style (16^th Edition):

Ahmed, Ahmed. “Nitrogen Abundances in Early-Type Be Stars.” 2015. Thesis, University of Western Ontario. Accessed March 07, 2021. https://ir.lib.uwo.ca/etd/3354.

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

MLA Handbook (7^th Edition):

Ahmed, Ahmed. “Nitrogen Abundances in Early-Type Be Stars.” 2015. Web. 07 Mar 2021.

Vancouver:

Ahmed A. Nitrogen Abundances in Early-Type Be Stars. [Internet] [Thesis]. University of Western Ontario; 2015. [cited 2021 Mar 07]. Available from: https://ir.lib.uwo.ca/etd/3354.

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

Council of Science Editors:

Ahmed A. Nitrogen Abundances in Early-Type Be Stars. [Thesis]. University of Western Ontario; 2015. Available from: https://ir.lib.uwo.ca/etd/3354

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

7. Mirouh, Giovanni Marcello. Rôle de la rotation différentielle sur le spectre basse fréquence des étoiles en rotation rapide : Role of differential rotation on low-frequency oscillation spectra of fast-rotating stars.

Degree: Docteur es, Astrophysique, 2016, Université Toulouse III – Paul Sabatier

URL: http://www.theses.fr/2016TOU30374

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Les étoiles massives sont les principaux contributeurs à l'enrichissement du milieu interstellaire. Ce sont généralement des rotateurs rapides, dotés d'une enveloppe radiative dans laquelle l'interaction… (more)

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Les étoiles massives sont les principaux contributeurs à l'enrichissement du milieu interstellaire. Ce sont généralement des rotateurs rapides, dotés d'une enveloppe radiative dans laquelle l'interaction de la stratification et la rotation génère une rotation différentielle. Celle-ci peut alimenter divers phénomènes de transport et l'évolution rapide de l'étoile. Nombre de ces étoiles sont par ailleurs des pulsateurs classiques. Cette thèse s'intéresse en premier lieu à l'interaction entre la rotation différentielle et les pulsations à basse fréquence dans l'étoile : celles-ci sont des modes gravito-inertiels dont la force de rappel est une combinaison de la force de Coriolis et de la poussée d'Archimède. Ils sondent les couches profondes de l'étoile, et sont étudiés suivant deux méthodes : dans la limite non-dissipative par la méthode des caractéristiques, et dans le cas dissipatif par la résolution du problème complet par une méthode spectrale. Nous mettons en évidence différentes singularités (attracteurs, latitudes critiques, résonances de corotation, piégeage en coin) et des modes réguliers. Certains modes sont excités par des instabilités baroclines, qui, si des effets non-linéaires provoquent leur saturation, permettent l'existence d'un mécanisme d'excitation nouveau dû à la rotation différentielle. Dans un second temps, nous avons associé le code de structure ESTER au code de calcul d'oscillations TOP. Ces deux codes calculent les quantités dans une étoile en deux dimensions et les modes associés en tenant compte des effets de la rotation de façon complète. Nous utilisons visibilités et taux d'amortissement des modes pour sélectionner dans le spectre synthétique les meilleurs candidats à l'identification des modes observés. Nous présentons une application au rotateur rapide Rasalhague (aOph), pour lequel de nombreuses observations sont disponibles. Nous n'avons pas obtenu une identification des modes univoque, mais le problème est maintenant mieux cerné et diverses pistes de progrès ont été identifiées.

Massive stars are the main contributors of the interstellar medium enrichment. These stars are usually fast rotators, with a radiative envelope in which the interaction between stratification and rotation gives rise to a differential rotation. This can trigger transport phenomena in the star, and affect its fast evolution. Besides, many of these stars are classical pulsators. This work focuses first on the impact of a differential rotation on the low-frequency oscillation spectrum which contains gravito-inertial modes. These modes are restored by the combination of buoyancy and Coriolis force and probe deep layers of stars. Our study is twofold : we compute the paths of characteristics in the non-dissipative limit, and solve the fully-dissipative eigenvalue problem numerically using a spectral decomposition. We find various singularities (attractors, critical latitudes, corotation resonances, wedge-trapping) and regular modes. Some of these modes are excited by baroclinic instabilities that may saturate…

Advisors/Committee Members: Rieutord, Michel (thesis director), Ballot, Jérôme (thesis director).

Subjects/Keywords: Etoiles; Oscillations stellaires; Etoiles en rotation; Rotation différentielle; Astérosismologie; Instabilités; Stars; Stellar pulsations; Stellar rotation; Differential rotation; Asteroseismology; Baroclinic instabilities

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APA · Chicago · MLA · Vancouver · CSE | Export to Zotero / EndNote / Reference Manager

APA (6^th Edition):

Mirouh, G. M. (2016). Rôle de la rotation différentielle sur le spectre basse fréquence des étoiles en rotation rapide : Role of differential rotation on low-frequency oscillation spectra of fast-rotating stars. (Doctoral Dissertation). Université Toulouse III – Paul Sabatier. Retrieved from http://www.theses.fr/2016TOU30374

Chicago Manual of Style (16^th Edition):

Mirouh, Giovanni Marcello. “Rôle de la rotation différentielle sur le spectre basse fréquence des étoiles en rotation rapide : Role of differential rotation on low-frequency oscillation spectra of fast-rotating stars.” 2016. Doctoral Dissertation, Université Toulouse III – Paul Sabatier. Accessed March 07, 2021. http://www.theses.fr/2016TOU30374.

MLA Handbook (7^th Edition):

Mirouh, Giovanni Marcello. “Rôle de la rotation différentielle sur le spectre basse fréquence des étoiles en rotation rapide : Role of differential rotation on low-frequency oscillation spectra of fast-rotating stars.” 2016. Web. 07 Mar 2021.

Vancouver:

Mirouh GM. Rôle de la rotation différentielle sur le spectre basse fréquence des étoiles en rotation rapide : Role of differential rotation on low-frequency oscillation spectra of fast-rotating stars. [Internet] [Doctoral dissertation]. Université Toulouse III – Paul Sabatier; 2016. [cited 2021 Mar 07]. Available from: http://www.theses.fr/2016TOU30374.

Council of Science Editors:

Mirouh GM. Rôle de la rotation différentielle sur le spectre basse fréquence des étoiles en rotation rapide : Role of differential rotation on low-frequency oscillation spectra of fast-rotating stars. [Doctoral Dissertation]. Université Toulouse III – Paul Sabatier; 2016. Available from: http://www.theses.fr/2016TOU30374

Universidade do Rio Grande do Norte

8. Maciel, Saulo Carneiro. Uma análise teórica da evolução da rotação estelar .

Degree: 2007, Universidade do Rio Grande do Norte

URL: http://repositorio.ufrn.br/handle/123456789/16525

► In the past 50 years, large eﬀorts have been made toward the understanding of the stellar evolution. In the observational context, large sets of precise… (more)

Subjects/Keywords: Rotação; Estrelas subgigantes; Estrelas gigantes; Análise teórica; Rotation; Subgiants stars; Giants stars; Theoretical analysis

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APA (6^th Edition):

Maciel, S. C. (2007). Uma análise teórica da evolução da rotação estelar . (Thesis). Universidade do Rio Grande do Norte. Retrieved from http://repositorio.ufrn.br/handle/123456789/16525

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

Chicago Manual of Style (16^th Edition):

Maciel, Saulo Carneiro. “Uma análise teórica da evolução da rotação estelar .” 2007. Thesis, Universidade do Rio Grande do Norte. Accessed March 07, 2021. http://repositorio.ufrn.br/handle/123456789/16525.

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

MLA Handbook (7^th Edition):

Maciel, Saulo Carneiro. “Uma análise teórica da evolução da rotação estelar .” 2007. Web. 07 Mar 2021.

Vancouver:

Maciel SC. Uma análise teórica da evolução da rotação estelar . [Internet] [Thesis]. Universidade do Rio Grande do Norte; 2007. [cited 2021 Mar 07]. Available from: http://repositorio.ufrn.br/handle/123456789/16525.

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

Council of Science Editors:

Maciel SC. Uma análise teórica da evolução da rotação estelar . [Thesis]. Universidade do Rio Grande do Norte; 2007. Available from: http://repositorio.ufrn.br/handle/123456789/16525

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

9. Pinçon, Charly. Du transport de moment cinétique par les ondes internes de gravité à l'heure de la sismologie stellaire : On the angular momentum transport by internal gravity waves at the time of asteroseismology.

Degree: Docteur es, Astronomie et Astrophysique, 2017, Paris Sciences et Lettres (ComUE)

URL: http://www.theses.fr/2017PSLEO009

► Les missions spatiales CoRoT (2006-2014) et Kepler (2009) ont procuré de nombreuses données sismiques pour des milliers d'étoiles de faible masse. L'analyse de ces données… (more)

▼ Les missions spatiales CoRoT (2006-2014) et Kepler (2009) ont procuré de nombreuses données sismiques pour des milliers d'étoiles de faible masse. L'analyse de ces données a rendu possible l'étude de l'intérieur de ces étoiles au cours de l'évolution et a apporté de fortes contraintes sur les processus physiques à l’œuvre sous leur surface. En particulier, ces observations ont montré que la rotation moyenne du cœur de ces étoiles augmente légèrement avec le temps sur la branche des sous-géantes avant de diminuer lors de l'ascension de la branche des géantes rouges. Ceci est désaccord avec les prédictions théoriques actuelles et souligne la nécessité d'inclure de nouveaux processus de transport de moment cinétique dans les modèles stellaires. Dans une première partie, j'ai donc étudié l'influence du transport de moment cinétique par les ondes internes de gravité sur l'évolution de la rotation dans les étoiles de faible masse. Ces ondes se propagent dans les zones radiatives stablement stratifiées et sont capables d'en modifier la vitesse de rotation moyenne. Or, l'efficacité du transport par les ondes dépend de leur amplitude et donc du mécanisme d'excitation. Alors que des modèles semi-analytiques permettaient déjà d'évaluer l'énergie transférée aux ondes par la pression turbulente dans la zone convective, une estimation théorique de l'excitation par la pénétration de panaches convectifs à l'interface avec la zone radiative restait manquante. J'ai donc proposé un modèle d'excitation pour estimer la part d'énergie cinétique des panaches transférées sous forme d'ondes à la base de la zone convective (Pinçon et al., 2016). Cela m'a d'abord permis d'établir que la pénétration convective génère des ondes plus efficacement que la pression turbulente, et ensuite que les ondes induites par la pénétration convective sont capables de s'opposer à l'accélération de la rotation due à la contraction des couches internes, depuis la séquence principale jusqu'au début de l'ascension de la branche des géantes rouges. En particulier, j'ai montré que les valeurs de la rotation observées dans l'intérieur des étoiles sous-géantes peuvent être interprétées comme le possible résultat d'un mécanisme de régulation contrôlé par ces ondes (Pinçon at al., 2017). Dans une seconde partie, je me suis intéressé à l'amélioration et à l'élaboration des diagnostiques sismiques par les modes mixtes, ces modes d'oscillation qui sont capables de sonder aussi bien l'enveloppe que les régions centrales des étoiles. Les diagnostiques sismiques font le lien entre les caractéristiques observées dans un spectre d'oscillation et les propriétés de la structure interne de l'étoile. Mon attention s'est premièrement focalisée sur la facteur de couplage des modes mixtes qui décrit le degré d'interaction entre les oscillations dans la cavité centrale et celles dans l'enveloppe de l'étoile. Ce paramètre n'a été, jusque là, que très peu étudié. Une première étude observationnelle sur un large échantillon d'étoiles par Mosser et al. (2017) a montré que ce facteur varie… Advisors/Committee Members: Goupil, Marie-Jo (thesis director), Belkacem, Kevin (thesis director).

Subjects/Keywords: Étoiles; Évolution; Rotation; Astérosismologie; Ondes; Hydrodynamique; Stars; Evolution; Rotation; Asteroseismology; Waves; Hydrodynamics; 520

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APA · Chicago · MLA · Vancouver · CSE | Export to Zotero / EndNote / Reference Manager

APA (6^th Edition):

Pinçon, C. (2017). Du transport de moment cinétique par les ondes internes de gravité à l'heure de la sismologie stellaire : On the angular momentum transport by internal gravity waves at the time of asteroseismology. (Doctoral Dissertation). Paris Sciences et Lettres (ComUE). Retrieved from http://www.theses.fr/2017PSLEO009

Chicago Manual of Style (16^th Edition):

Pinçon, Charly. “Du transport de moment cinétique par les ondes internes de gravité à l'heure de la sismologie stellaire : On the angular momentum transport by internal gravity waves at the time of asteroseismology.” 2017. Doctoral Dissertation, Paris Sciences et Lettres (ComUE). Accessed March 07, 2021. http://www.theses.fr/2017PSLEO009.

MLA Handbook (7^th Edition):

Pinçon, Charly. “Du transport de moment cinétique par les ondes internes de gravité à l'heure de la sismologie stellaire : On the angular momentum transport by internal gravity waves at the time of asteroseismology.” 2017. Web. 07 Mar 2021.

Vancouver:

Pinçon C. Du transport de moment cinétique par les ondes internes de gravité à l'heure de la sismologie stellaire : On the angular momentum transport by internal gravity waves at the time of asteroseismology. [Internet] [Doctoral dissertation]. Paris Sciences et Lettres (ComUE); 2017. [cited 2021 Mar 07]. Available from: http://www.theses.fr/2017PSLEO009.

Council of Science Editors:

Pinçon C. Du transport de moment cinétique par les ondes internes de gravité à l'heure de la sismologie stellaire : On the angular momentum transport by internal gravity waves at the time of asteroseismology. [Doctoral Dissertation]. Paris Sciences et Lettres (ComUE); 2017. Available from: http://www.theses.fr/2017PSLEO009

10. Amard, Louis. Évolution de la rotation des étoiles jeunes de faible masse : Rotational evolution of young low-mass stars.

Degree: Docteur es, Physique, 2016, Montpellier; Observatoire de Genève (Suisse)

URL: http://www.theses.fr/2016MONTT258

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Le moment cinétique d’une étoile, comme sa masse ou sa composition chimique, est l’une de ses propriétés fondamentales, l’un de celles qui varient à cours… (more)

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Le moment cinétique d’une étoile, comme sa masse ou sa composition chimique, est l’une de ses propriétés fondamentales, l’un de celles qui varient à cours du temps et influent sur la structure de l’étoile. Celui-ci peut être global, on l’observe alors à travers la vitesse de rotation de surface d’une étoile, ou local, auquel cas il nous faut sonder l’intérieur stellaire et étudier les processus de redistribution au sein des régions internes du moment cinétique. Au cours de cette thèse dans le cadre du projet ToUpiES, nous nous sommes intéressés en particulier à l’évolution du moment cinétique des étoiles de faible masse au cours de leur jeunesse, qui est une période critique de leur vie en ce qui concerne l’impact et l’évolution du moment cinétique. Nous avons d’abord inclus au sein du code d’évolution STAREVOL les prescriptions les plus à jour pour l’extraction du moment cinétique par les vents magnétisés. L’étude systématique des combinaisons de ce freinage avec différentes prescriptions existantes pour le traitement de la turbulence horizontale et verticale dans la zone radiative des étoiles, nous a permis de sélectionner un jeu de prescriptions capable de reproduire, les périodes de rotation dans les amas ouverts pour une étoile de type solaire. Nous comparons ensuite l’application de ces processus de transport et d’extraction du moment cinétique à un modèle de 1, 2 masse solaire, aux autres processus jugés potentiellement efficaces pour transport le moment cinétique à ce jour (ondes internes de gravités, instabilité MHD de Tayler-Spruit, modes de gravités). Cela nous a permis de présenter dans chacun des cas les spécificités du profil de rotation prédit par ces différents modes de transport. Puis, nous avons mis en place un modèle rotationnel fonctionnel adapté à l’ensemble des étoiles de faible masse, permettant entre autre de reproduire les périodes de rotation observées dans les amas jeunes pour les étoiles de faible masse (avec une masse comprise entre 0, 2 et 1, 1 M⊙). Ceci a donné lieu à une grille de modèle d’évolution unique à ce jour. Enfin, cette grille a été utilisée dans le cadre de travaux dans différents domaines, tels que l’impact de l’évolution stellaire sur l’habitabilité d’un système, la caractérisation d’étoiles-hôte ou encore l’étude de l’évolution de la topologie magnétique au cours des phases jeunes.

The angular momentum content of a star, as its mass or its chemical composition is one of the fundamental properties of a star, one of those that evolves with time and modify the stellar structure. The angular momentum can be studied as a global property, we can then observe it through the surface rotation velocity, or a local property that vary inside the star, we therefore have to probe the stellar radiation zone and study the secular angular momentum redistribution processes that happen in this region. During this PhD, in the frame of the ToUpiES project, we have been especially interested in the evolution of the…

Advisors/Committee Members: Palacios, Ana (thesis director), Charbonnel, Corinne (thesis director).

Subjects/Keywords: Evolution stellaire; Rotation; Magnétohydrodynamique; Etoiles jeunes; Stellar Evolution; Rotation; Young stars; Magnetohydrodynamics

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APA (6^th Edition):

Amard, L. (2016). Évolution de la rotation des étoiles jeunes de faible masse : Rotational evolution of young low-mass stars. (Doctoral Dissertation). Montpellier; Observatoire de Genève (Suisse). Retrieved from http://www.theses.fr/2016MONTT258

Chicago Manual of Style (16^th Edition):

Amard, Louis. “Évolution de la rotation des étoiles jeunes de faible masse : Rotational evolution of young low-mass stars.” 2016. Doctoral Dissertation, Montpellier; Observatoire de Genève (Suisse). Accessed March 07, 2021. http://www.theses.fr/2016MONTT258.

MLA Handbook (7^th Edition):

Amard, Louis. “Évolution de la rotation des étoiles jeunes de faible masse : Rotational evolution of young low-mass stars.” 2016. Web. 07 Mar 2021.

Vancouver:

Amard L. Évolution de la rotation des étoiles jeunes de faible masse : Rotational evolution of young low-mass stars. [Internet] [Doctoral dissertation]. Montpellier; Observatoire de Genève (Suisse); 2016. [cited 2021 Mar 07]. Available from: http://www.theses.fr/2016MONTT258.

Council of Science Editors:

Amard L. Évolution de la rotation des étoiles jeunes de faible masse : Rotational evolution of young low-mass stars. [Doctoral Dissertation]. Montpellier; Observatoire de Genève (Suisse); 2016. Available from: http://www.theses.fr/2016MONTT258

University of Alberta

11. Couture, Claudine. Orbital influence of the oscillations excited inside a rotating star in a binary system.

Degree: MS, Department of Physics, 2002, University of Alberta

URL: https://era.library.ualberta.ca/files/dn39x313m

Subjects/Keywords: Stars – Rotation.; Stars – Orbits.; Equations of motion.; Neutron stars.

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APA (6^th Edition):

Couture, C. (2002). Orbital influence of the oscillations excited inside a rotating star in a binary system. (Masters Thesis). University of Alberta. Retrieved from https://era.library.ualberta.ca/files/dn39x313m

Chicago Manual of Style (16^th Edition):

Couture, Claudine. “Orbital influence of the oscillations excited inside a rotating star in a binary system.” 2002. Masters Thesis, University of Alberta. Accessed March 07, 2021. https://era.library.ualberta.ca/files/dn39x313m.

MLA Handbook (7^th Edition):

Couture, Claudine. “Orbital influence of the oscillations excited inside a rotating star in a binary system.” 2002. Web. 07 Mar 2021.

Vancouver:

Couture C. Orbital influence of the oscillations excited inside a rotating star in a binary system. [Internet] [Masters thesis]. University of Alberta; 2002. [cited 2021 Mar 07]. Available from: https://era.library.ualberta.ca/files/dn39x313m.

Council of Science Editors:

Couture C. Orbital influence of the oscillations excited inside a rotating star in a binary system. [Masters Thesis]. University of Alberta; 2002. Available from: https://era.library.ualberta.ca/files/dn39x313m

12. André, Quentin. Ondes gravito-inertielles dans les étoiles et les planètes géantes : propagation, dissipation et échanges de moment cinétique : Gravito-inertial waves in stars and giant planets : propagation, dissipation and angular momentum transport.

Degree: Docteur es, Physique. Astronomie et astrophysique, 2019, Université de Paris (2019-....)

URL: http://www.theses.fr/2019UNIP7073

► Les ondes internes gravito-inertielles sont des ondes se propageant dans les milieux fluides stablement stratifiés en rotation. Leurs forces de rappel sont la poussée d'Archimède… (more)

▼ Les ondes internes gravito-inertielles sont des ondes se propageant dans les milieux fluides stablement stratifiés en rotation. Leurs forces de rappel sont la poussée d'Archimède et l'accélération de Coriolis. Elles sont capables de redistribuer de l'énergie et du moment cinétique du fait de leur dissipation et de leur possible déferlement non-linéaire, jouant ainsi un rôle crucial dans l’évolution dynamique des corps dans lesquels elles se propagent. Dans cette thèse, nous nous attachons à caractériser leur propagation, leur amortissement et les échanges de moment cinétique qu’elles induisent, dans les environnements complexes que sont les intérieurs stellaires et de planètes géantes.Au sein des planètes géantes, nous étudions la propagation et la dissipation d’ondes gravito-inertielles de marée, dans une région de convection stratifiée susceptible de se développer proche du cœur. Nous nous intéressons tout d’abord à leur propagation libre et nous montrons qu’une onde incidente sur une telle région est efficacement transmise à condition qu’elle soit résonante avec un de ses modes propres. Sinon, l’onde est réfléchie et ne pénètre pas dans les régions plus profondes de la planète. Ensuite, nous étudions numériquement la dissipation de marée induite lorsque ces ondes sont excitées par un forçage gravitationnel dû à la présence d’un satellite. Nous montrons que le taux de dissipation de marée est en moyenne augmenté par rapport à un milieu purement convectif. Les contributions les plus importantes à cette augmentation proviennent de la dissipation des ondes gravito-inertielles résonantes avec les modes propres de la région de convection stratifiée, qui sont aussi celles qui sont efficacement transmises. Ces résultats sont compatibles avec les hauts taux de dissipation de marée récemment observés dans Jupiter et Saturne.Dans les zones radiatives des étoiles, nous présentons en premier lieu une étude semi-analytique linéaire de l’influence de la rotation globale et différentielle, sur le transport de moment cinétique induit par la dissipation des ondes gravito-inertielles. Dans un modèle équatorial, nous montrons que la rotation a pour effet l’augmentation de la dissipation thermique des ondes. Celle-ci est particulièrement significative dans leur région d’excitation, modifiant ainsi le dépôt de moment cinétique. Nous montrons que cet effet se révèle d’autant plus efficace que l’étoile est jeune et massive. En parallèle de ce travail semi-analytique, cette thèse s’est attachée à développer un modèle 3D non-linéaire ab initio d’une étoile massive couplant le coeur convectif à une enveloppe radiative étendue, sous l’influence de la rotation. L’analyse détaillée de simulations numériques à haute performance, réalisées avec le code ASH, nous a permis de caractériser les propriétés du spectre d’excitation des ondes et des modes résonants qui s’établissent dans l’enveloppe radiative. Proche de la surface de l’étoile, nous montrons que les ondes peuvent atteindre une amplitude suffisante pour interagir de manière significative… Advisors/Committee Members: Mathis, Stéphane (thesis director), Brun, Allan Sacha (thesis director).

Subjects/Keywords: Interactions de marées; Hydrodynamics; Modelisation; Numerical simulation; Waves; Convection; Giant planets; Tides; Stars – Rotation; Stars – Evolution; Massive stars

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APA · Chicago · MLA · Vancouver · CSE | Export to Zotero / EndNote / Reference Manager

APA (6^th Edition):

André, Q. (2019). Ondes gravito-inertielles dans les étoiles et les planètes géantes : propagation, dissipation et échanges de moment cinétique : Gravito-inertial waves in stars and giant planets : propagation, dissipation and angular momentum transport. (Doctoral Dissertation). Université de Paris (2019-....). Retrieved from http://www.theses.fr/2019UNIP7073

Chicago Manual of Style (16^th Edition):

André, Quentin. “Ondes gravito-inertielles dans les étoiles et les planètes géantes : propagation, dissipation et échanges de moment cinétique : Gravito-inertial waves in stars and giant planets : propagation, dissipation and angular momentum transport.” 2019. Doctoral Dissertation, Université de Paris (2019-....). Accessed March 07, 2021. http://www.theses.fr/2019UNIP7073.

MLA Handbook (7^th Edition):

André, Quentin. “Ondes gravito-inertielles dans les étoiles et les planètes géantes : propagation, dissipation et échanges de moment cinétique : Gravito-inertial waves in stars and giant planets : propagation, dissipation and angular momentum transport.” 2019. Web. 07 Mar 2021.

Vancouver:

André Q. Ondes gravito-inertielles dans les étoiles et les planètes géantes : propagation, dissipation et échanges de moment cinétique : Gravito-inertial waves in stars and giant planets : propagation, dissipation and angular momentum transport. [Internet] [Doctoral dissertation]. Université de Paris (2019-....); 2019. [cited 2021 Mar 07]. Available from: http://www.theses.fr/2019UNIP7073.

Council of Science Editors:

André Q. Ondes gravito-inertielles dans les étoiles et les planètes géantes : propagation, dissipation et échanges de moment cinétique : Gravito-inertial waves in stars and giant planets : propagation, dissipation and angular momentum transport. [Doctoral Dissertation]. Université de Paris (2019-....); 2019. Available from: http://www.theses.fr/2019UNIP7073

University of Melbourne

13. PERALTA, CARLOS ANDRES. Superfluid spherical Couette flow and rotational irregularities in pulsars.

Degree: 2006, University of Melbourne

URL: http://hdl.handle.net/11343/39224

► Small amplitude rotational irregularities are observed in a number of rotation-powered pulsars. They fall into two classes: (i) glitches, defined as abrupt increases in the… (more)

Subjects/Keywords: dense matter; hydrodynamics; stars: interior; stars: neutron; stars: rotation

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APA · Chicago · MLA · Vancouver · CSE | Export to Zotero / EndNote / Reference Manager

APA (6^th Edition):

PERALTA, C. A. (2006). Superfluid spherical Couette flow and rotational irregularities in pulsars. (Doctoral Dissertation). University of Melbourne. Retrieved from http://hdl.handle.net/11343/39224

Chicago Manual of Style (16^th Edition):

PERALTA, CARLOS ANDRES. “Superfluid spherical Couette flow and rotational irregularities in pulsars.” 2006. Doctoral Dissertation, University of Melbourne. Accessed March 07, 2021. http://hdl.handle.net/11343/39224.

MLA Handbook (7^th Edition):

PERALTA, CARLOS ANDRES. “Superfluid spherical Couette flow and rotational irregularities in pulsars.” 2006. Web. 07 Mar 2021.

Vancouver:

PERALTA CA. Superfluid spherical Couette flow and rotational irregularities in pulsars. [Internet] [Doctoral dissertation]. University of Melbourne; 2006. [cited 2021 Mar 07]. Available from: http://hdl.handle.net/11343/39224.

Council of Science Editors:

PERALTA CA. Superfluid spherical Couette flow and rotational irregularities in pulsars. [Doctoral Dissertation]. University of Melbourne; 2006. Available from: http://hdl.handle.net/11343/39224

14. Harris, Amy. The kinematics of the outer Galactic disk from A and F stars.

Degree: PhD, 2019, University of Hertfordshire

URL: http://hdl.handle.net/2299/22451

► The kinematics of stars in the outer Galactic disk is poorly known. In addition to constraining the Galactic potential, knowledge of the motions of stars… (more)

▼ The kinematics of stars in the outer Galactic disk is poorly known. In addition to constraining the Galactic potential, knowledge of the motions of stars throughout the disk facilitates studies of non-axisymmetric motion, such as streaming motions due to spiral arms. Understanding the kinematics of the disk in full, including the rotation law, will help to map out its structure, and set constraints on its formation and evolution. I explore the kinematics of A/F stars in two outer-disk pencil beams. I show that A stars in particular are useful probes of outer Galactic disk kinematics. The use of these relatively early-type stars is an alternative to the ISM gas tracers and clump giants that have been commonly used in previous studies. A/F stars offer the advantage of reduced kinematic scatter and asymmetric drift as compared to the older clump giants, and can provide a much denser sampling in the outer disk than ISM gas tracers. They are bright so can be detected out to great distances, and large samples can be efficiently selected from the IPHAS r-i, r-Hα plane. The sightlines were chosen to sample the strong shear in Galactic rotation (l= 118 ̊), and as a control (l= 178 ̊). Radial velocities (RVs) and extinction-corrected spectro-photometric distances are computed for the sample of >1300 A/F stars with the aid of MCMC parameter fitting. The rotation law measured at l=118 ̊ using the RV data is sharply rising out from RG ~11 kpc, going against expectations of a flat or slowly rising law. Gaia DR2 astrometry, released in April 2018, provided proper motions for the sample. On combining these with the measured RVs and spectro-photometric distances, full space motions are obtained. The Galactocentric radial, azimuthal, and vertical velocity trends are constructed without any prior assumption about the velocity field. The measured rotation curve incorporating proper motion data is flat at l = 178 ̊, but remains sharply rising at l = 118 ̊, albeit less so than that determined using only RV data. I consider the detailed form of the observed Galactocentric trends with specific perturbers in mind, finding no clear interpretation in terms of perturbation from the central bar or spiral arms. The variation of observed trends with longitude and distance is a reflection of the complex dynamics in our Galaxy. The methods developed in this work and the use of A stars as tracers will be used in the future for fuller exploitation via spectroscopy on forthcoming massively multiplexed wide-field spectrographs. In particular, the PTMCMC method presented will be used to analyse WEAVE survey products. Future use of these young stellar tracers will help us to understand how our Galaxy is, and came to be, how it is now.

Subjects/Keywords: Astronomy; Astrophysics; Kinematics; Stars; Milky Way; Galaxy; galactic disk; rotation curve; young stars; massive stars; F stars; A stars; Dynamics; outer disk; Gaia; proper motion; radial velocity; spectroscopy

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APA · Chicago · MLA · Vancouver · CSE | Export to Zotero / EndNote / Reference Manager

APA (6^th Edition):

Harris, A. (2019). The kinematics of the outer Galactic disk from A and F stars. (Doctoral Dissertation). University of Hertfordshire. Retrieved from http://hdl.handle.net/2299/22451

Chicago Manual of Style (16^th Edition):

Harris, Amy. “The kinematics of the outer Galactic disk from A and F stars.” 2019. Doctoral Dissertation, University of Hertfordshire. Accessed March 07, 2021. http://hdl.handle.net/2299/22451.

MLA Handbook (7^th Edition):

Harris, Amy. “The kinematics of the outer Galactic disk from A and F stars.” 2019. Web. 07 Mar 2021.

Vancouver:

Harris A. The kinematics of the outer Galactic disk from A and F stars. [Internet] [Doctoral dissertation]. University of Hertfordshire; 2019. [cited 2021 Mar 07]. Available from: http://hdl.handle.net/2299/22451.

Council of Science Editors:

Harris A. The kinematics of the outer Galactic disk from A and F stars. [Doctoral Dissertation]. University of Hertfordshire; 2019. Available from: http://hdl.handle.net/2299/22451

15. Harris, Amy. The kinematics of the outer Galactic disk from A and F stars.

Degree: PhD, 2019, University of Hertfordshire

URL: https://doi.org/10.18745/th.22451 ; https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.802952

► The kinematics of stars in the outer Galactic disk is poorly known. In addition to constraining the Galactic potential, knowledge of the motions of stars… (more)

▼ The kinematics of stars in the outer Galactic disk is poorly known. In addition to constraining the Galactic potential, knowledge of the motions of stars throughout the disk facilitates studies of non-axisymmetric motion, such as streaming motions due to spiral arms. Understanding the kinematics of the disk in full, including the rotation law, will help to map out its structure, and set constraints on its formation and evolution. I explore the kinematics of A/F stars in two outer-disk pencil beams. I show that A stars in particular are useful probes of outer Galactic disk kinematics. The use of these relatively early-type stars is an alternative to the ISM gas tracers and clump giants that have been commonly used in previous studies. A/F stars offer the advantage of reduced kinematic scatter and asymmetric drift as compared to the older clump giants, and can provide a much denser sampling in the outer disk than ISM gas tracers. They are bright so can be detected out to great distances, and large samples can be efficiently selected from the IPHAS r-i, r-Hα plane. The sightlines were chosen to sample the strong shear in Galactic rotation (l= 118 ̊), and as a control (l= 178 ̊). Radial velocities (RVs) and extinction-corrected spectro-photometric distances are computed for the sample of >1300 A/F stars with the aid of MCMC parameter fitting. The rotation law measured at l=118 ̊ using the RV data is sharply rising out from RG ~11 kpc, going against expectations of a flat or slowly rising law. Gaia DR2 astrometry, released in April 2018, provided proper motions for the sample. On combining these with the measured RVs and spectro-photometric distances, full space motions are obtained. The Galactocentric radial, azimuthal, and vertical velocity trends are constructed without any prior assumption about the velocity field. The measured rotation curve incorporating proper motion data is flat at l = 178 ̊, but remains sharply rising at l = 118 ̊, albeit less so than that determined using only RV data. I consider the detailed form of the observed Galactocentric trends with specific perturbers in mind, finding no clear interpretation in terms of perturbation from the central bar or spiral arms. The variation of observed trends with longitude and distance is a reflection of the complex dynamics in our Galaxy. The methods developed in this work and the use of A stars as tracers will be used in the future for fuller exploitation via spectroscopy on forthcoming massively multiplexed wide-field spectrographs. In particular, the PTMCMC method presented will be used to analyse WEAVE survey products. Future use of these young stellar tracers will help us to understand how our Galaxy is, and came to be, how it is now.

Subjects/Keywords: Astronomy; Astrophysics; Kinematics; Stars; Milky Way; Galaxy; galactic disk; rotation curve; young stars; massive stars; F stars; A stars; Dynamics; outer disk; Gaia; proper motion; radial velocity; spectroscopy

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APA · Chicago · MLA · Vancouver · CSE | Export to Zotero / EndNote / Reference Manager

APA (6^th Edition):

Harris, A. (2019). The kinematics of the outer Galactic disk from A and F stars. (Doctoral Dissertation). University of Hertfordshire. Retrieved from https://doi.org/10.18745/th.22451 ; https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.802952

Chicago Manual of Style (16^th Edition):

Harris, Amy. “The kinematics of the outer Galactic disk from A and F stars.” 2019. Doctoral Dissertation, University of Hertfordshire. Accessed March 07, 2021. https://doi.org/10.18745/th.22451 ; https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.802952.

MLA Handbook (7^th Edition):

Harris, Amy. “The kinematics of the outer Galactic disk from A and F stars.” 2019. Web. 07 Mar 2021.

Vancouver:

Harris A. The kinematics of the outer Galactic disk from A and F stars. [Internet] [Doctoral dissertation]. University of Hertfordshire; 2019. [cited 2021 Mar 07]. Available from: https://doi.org/10.18745/th.22451 ; https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.802952.

Council of Science Editors:

Harris A. The kinematics of the outer Galactic disk from A and F stars. [Doctoral Dissertation]. University of Hertfordshire; 2019. Available from: https://doi.org/10.18745/th.22451 ; https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.802952

16. Potter, Adrian Thomas. Rotation and magnetism in massive stars.

Degree: PhD, 2012, University of Cambridge

URL: http://www.dspace.cam.ac.uk/handle/1810/243617https://www.repository.cam.ac.uk/bitstream/1810/243617/2/license.txt ; https://www.repository.cam.ac.uk/bitstream/1810/243617/3/license_url ; https://www.repository.cam.ac.uk/bitstream/1810/243617/4/license_text ; https://www.repository.cam.ac.uk/bitstream/1810/243617/5/license_rdf ; https://www.repository.cam.ac.uk/bitstream/1810/243617/9/potterThesis.pdf.txt ; https://www.repository.cam.ac.uk/bitstream/1810/243617/7/potterThesis.pdf.txt ; https://www.repository.cam.ac.uk/bitstream/1810/243617/10/potterThesis.pdf.jpg

► Rotation has a number of important effects on the evolution of stars. Apart from structural changes because of the centrifugal force, turbulent mixing and meridional… (more)

▼ Rotation has a number of important effects on the evolution of stars. Apart from structural changes because of the centrifugal force, turbulent mixing and meridional circulation can dramatically affect a star's chemical evolution. This leads to changes in the surface temperature and luminosity as well as modifying its lifetime. Rotation decreases the surface gravity, causes enhanced mass loss and leads to surface abundance anomalies of various chemical isotopes all of which have been observed. The replication of these physical effects with simple stellar evolution models is very difficult and has resulted in the use of numerous different formulations to describe the physics. We have adapted the Cambridge stellar evolution code to incorporate a number of different physical models for rotation, including several treatments of angular momentum transport in convection zones. We compare detailed grids of stellar evolution models along with simulated stellar populations to identify the key differences between them. We then consider how these models relate to observed data. Models of rotationally-driven dynamos in stellar radiative zones have suggested that magnetohydrodynamic transport of angular momentum and chemical composition can dominate over the otherwise purely hydrodynamic processes. If this is the case then a proper consideration of the interaction between rotation and magnetic fields is essential. We have adapted our purely hydrodynamic model to include the evolution of the magnetic field with a pair of time-dependent advection – diffusion equations coupled with the equations for the evolution of the angular momentum distribution and stellar structure. This produces a much more complete, though still reasonably simple, model for the magnetic field evolution. We consider how the surface field strength varies during the main-sequence evolution and compare the surface enrichment of nitrogen for a simulated stellar population with observations. Strong magnetic fields are also observed at the end of the stellar lifetime. The surface magnetic field strength of white dwarfs is observed to vary from very little up to 10^9G. As well as considering the main-sequence evolution of magnetic fields we also look at how the strongest magnetic fields in white dwarfs may be generated by dynamo action during the common envelope phase of strongly interacting binary stars. The resulting magnetic field depends strongly on the electrical conductivity of the white dwarf, the lifetime of the convective envelope and the variability of the magnetic dynamo. We assess the various energy sources available and estimate necessary lifetimes of the common envelope.

Subjects/Keywords: Stars; Astronomy; Rotation; Magnetic; Chemically peculiar; Evolution; Stellar

10 more images…

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APA · Chicago · MLA · Vancouver · CSE | Export to Zotero / EndNote / Reference Manager

APA (6^th Edition):

Potter, A. T. (2012). Rotation and magnetism in massive stars. (Doctoral Dissertation). University of Cambridge. Retrieved from http://www.dspace.cam.ac.uk/handle/1810/243617https://www.repository.cam.ac.uk/bitstream/1810/243617/2/license.txt ; https://www.repository.cam.ac.uk/bitstream/1810/243617/3/license_url ; https://www.repository.cam.ac.uk/bitstream/1810/243617/4/license_text ; https://www.repository.cam.ac.uk/bitstream/1810/243617/5/license_rdf ; https://www.repository.cam.ac.uk/bitstream/1810/243617/9/potterThesis.pdf.txt ; https://www.repository.cam.ac.uk/bitstream/1810/243617/7/potterThesis.pdf.txt ; https://www.repository.cam.ac.uk/bitstream/1810/243617/10/potterThesis.pdf.jpg

Chicago Manual of Style (16^th Edition):

Potter, Adrian Thomas. “Rotation and magnetism in massive stars.” 2012. Doctoral Dissertation, University of Cambridge. Accessed March 07, 2021. http://www.dspace.cam.ac.uk/handle/1810/243617https://www.repository.cam.ac.uk/bitstream/1810/243617/2/license.txt ; https://www.repository.cam.ac.uk/bitstream/1810/243617/3/license_url ; https://www.repository.cam.ac.uk/bitstream/1810/243617/4/license_text ; https://www.repository.cam.ac.uk/bitstream/1810/243617/5/license_rdf ; https://www.repository.cam.ac.uk/bitstream/1810/243617/9/potterThesis.pdf.txt ; https://www.repository.cam.ac.uk/bitstream/1810/243617/7/potterThesis.pdf.txt ; https://www.repository.cam.ac.uk/bitstream/1810/243617/10/potterThesis.pdf.jpg.

MLA Handbook (7^th Edition):

Potter, Adrian Thomas. “Rotation and magnetism in massive stars.” 2012. Web. 07 Mar 2021.

Vancouver:

Potter AT. Rotation and magnetism in massive stars. [Internet] [Doctoral dissertation]. University of Cambridge; 2012. [cited 2021 Mar 07]. Available from: http://www.dspace.cam.ac.uk/handle/1810/243617https://www.repository.cam.ac.uk/bitstream/1810/243617/2/license.txt ; https://www.repository.cam.ac.uk/bitstream/1810/243617/3/license_url ; https://www.repository.cam.ac.uk/bitstream/1810/243617/4/license_text ; https://www.repository.cam.ac.uk/bitstream/1810/243617/5/license_rdf ; https://www.repository.cam.ac.uk/bitstream/1810/243617/9/potterThesis.pdf.txt ; https://www.repository.cam.ac.uk/bitstream/1810/243617/7/potterThesis.pdf.txt ; https://www.repository.cam.ac.uk/bitstream/1810/243617/10/potterThesis.pdf.jpg.

Council of Science Editors:

Potter AT. Rotation and magnetism in massive stars. [Doctoral Dissertation]. University of Cambridge; 2012. Available from: http://www.dspace.cam.ac.uk/handle/1810/243617https://www.repository.cam.ac.uk/bitstream/1810/243617/2/license.txt ; https://www.repository.cam.ac.uk/bitstream/1810/243617/3/license_url ; https://www.repository.cam.ac.uk/bitstream/1810/243617/4/license_text ; https://www.repository.cam.ac.uk/bitstream/1810/243617/5/license_rdf ; https://www.repository.cam.ac.uk/bitstream/1810/243617/9/potterThesis.pdf.txt ; https://www.repository.cam.ac.uk/bitstream/1810/243617/7/potterThesis.pdf.txt ; https://www.repository.cam.ac.uk/bitstream/1810/243617/10/potterThesis.pdf.jpg

University of Toronto

17. Kissin, Yevgeni. Properties of Stellar Remnants: Rotational and Magnetic Evolution of Their Progenitors.

Degree: PhD, 2017, University of Toronto

URL: http://hdl.handle.net/1807/80715

► The rotation and magnetic evolution of stars is examined in detail. Advection of angular momentum by convective plumes is a source of differential rotation, which… (more)

Subjects/Keywords: Black holes; Magnetic fields; Neutron stars; Rotation; White dwarfs; 0596

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APA (6^th Edition):

Kissin, Y. (2017). Properties of Stellar Remnants: Rotational and Magnetic Evolution of Their Progenitors. (Doctoral Dissertation). University of Toronto. Retrieved from http://hdl.handle.net/1807/80715

Chicago Manual of Style (16^th Edition):

Kissin, Yevgeni. “Properties of Stellar Remnants: Rotational and Magnetic Evolution of Their Progenitors.” 2017. Doctoral Dissertation, University of Toronto. Accessed March 07, 2021. http://hdl.handle.net/1807/80715.

MLA Handbook (7^th Edition):

Kissin, Yevgeni. “Properties of Stellar Remnants: Rotational and Magnetic Evolution of Their Progenitors.” 2017. Web. 07 Mar 2021.

Vancouver:

Kissin Y. Properties of Stellar Remnants: Rotational and Magnetic Evolution of Their Progenitors. [Internet] [Doctoral dissertation]. University of Toronto; 2017. [cited 2021 Mar 07]. Available from: http://hdl.handle.net/1807/80715.

Council of Science Editors:

Kissin Y. Properties of Stellar Remnants: Rotational and Magnetic Evolution of Their Progenitors. [Doctoral Dissertation]. University of Toronto; 2017. Available from: http://hdl.handle.net/1807/80715

University of Cambridge

18. Potter, Adrian Thomas. Rotation and magnetism in massive stars.

Degree: PhD, 2012, University of Cambridge

URL: https://doi.org/10.17863/CAM.15999 ; https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.556241

► Rotation has a number of important effects on the evolution of stars. Apart from structural changes because of the centrifugal force, turbulent mixing and meridional… (more)

▼ Rotation has a number of important effects on the evolution of stars. Apart from structural changes because of the centrifugal force, turbulent mixing and meridional circulation can dramatically affect a star's chemical evolution. This leads to changes in the surface temperature and luminosity as well as modifying its lifetime. Rotation decreases the surface gravity, causes enhanced mass loss and leads to surface abundance anomalies of various chemical isotopes all of which have been observed. The replication of these physical effects with simple stellar evolution models is very difficult and has resulted in the use of numerous different formulations to describe the physics. We have adapted the Cambridge stellar evolution code to incorporate a number of different physical models for rotation, including several treatments of angular momentum transport in convection zones. We compare detailed grids of stellar evolution models along with simulated stellar populations to identify the key differences between them. We then consider how these models relate to observed data. Models of rotationally-driven dynamos in stellar radiative zones have suggested that magnetohydrodynamic transport of angular momentum and chemical composition can dominate over the otherwise purely hydrodynamic processes. If this is the case then a proper consideration of the interaction between rotation and magnetic fields is essential. We have adapted our purely hydrodynamic model to include the evolution of the magnetic field with a pair of time-dependent advection – diffusion equations coupled with the equations for the evolution of the angular momentum distribution and stellar structure. This produces a much more complete, though still reasonably simple, model for the magnetic field evolution. We consider how the surface field strength varies during the main-sequence evolution and compare the surface enrichment of nitrogen for a simulated stellar population with observations. Strong magnetic fields are also observed at the end of the stellar lifetime. The surface magnetic field strength of white dwarfs is observed to vary from very little up to 10 9G. As well as considering the main-sequence evolution of magnetic fields we also look at how the strongest magnetic fields in white dwarfs may be generated by dynamo action during the common envelope phase of strongly interacting binary stars. The resulting magnetic field depends strongly on the electrical conductivity of the white dwarf, the lifetime of the convective envelope and the variability of the magnetic dynamo. We assess the various energy sources available and estimate necessary lifetimes of the common envelope.

Subjects/Keywords: 520; Stars; Astronomy; Rotation; Magnetic; Chemically peculiar; Evolution; Stellar

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APA (6^th Edition):

Potter, A. T. (2012). Rotation and magnetism in massive stars. (Doctoral Dissertation). University of Cambridge. Retrieved from https://doi.org/10.17863/CAM.15999 ; https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.556241

Chicago Manual of Style (16^th Edition):

Potter, Adrian Thomas. “Rotation and magnetism in massive stars.” 2012. Doctoral Dissertation, University of Cambridge. Accessed March 07, 2021. https://doi.org/10.17863/CAM.15999 ; https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.556241.

MLA Handbook (7^th Edition):

Potter, Adrian Thomas. “Rotation and magnetism in massive stars.” 2012. Web. 07 Mar 2021.

Vancouver:

Potter AT. Rotation and magnetism in massive stars. [Internet] [Doctoral dissertation]. University of Cambridge; 2012. [cited 2021 Mar 07]. Available from: https://doi.org/10.17863/CAM.15999 ; https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.556241.

Council of Science Editors:

Potter AT. Rotation and magnetism in massive stars. [Doctoral Dissertation]. University of Cambridge; 2012. Available from: https://doi.org/10.17863/CAM.15999 ; https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.556241

The Ohio State University

19. Tayar, Jamie Nicole. Rotation in Red Giants.

Degree: PhD, Astronomy, 2018, The Ohio State University

URL: http://rave.ohiolink.edu/etdc/view?acc_num=osu1531927526281553

► Real stars rotate, and rotation can have profound consequences for stellar structure and evolution. Despite this, rotation is frequently ignored in evolved stars, or treated… (more)

Subjects/Keywords: Astronomy; stars; stellar evolution; stellar rotation; red giants

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APA · Chicago · MLA · Vancouver · CSE | Export to Zotero / EndNote / Reference Manager

APA (6^th Edition):

Tayar, J. N. (2018). Rotation in Red Giants. (Doctoral Dissertation). The Ohio State University. Retrieved from http://rave.ohiolink.edu/etdc/view?acc_num=osu1531927526281553

Chicago Manual of Style (16^th Edition):

Tayar, Jamie Nicole. “Rotation in Red Giants.” 2018. Doctoral Dissertation, The Ohio State University. Accessed March 07, 2021. http://rave.ohiolink.edu/etdc/view?acc_num=osu1531927526281553.

MLA Handbook (7^th Edition):

Tayar, Jamie Nicole. “Rotation in Red Giants.” 2018. Web. 07 Mar 2021.

Vancouver:

Tayar JN. Rotation in Red Giants. [Internet] [Doctoral dissertation]. The Ohio State University; 2018. [cited 2021 Mar 07]. Available from: http://rave.ohiolink.edu/etdc/view?acc_num=osu1531927526281553.

Council of Science Editors:

Tayar JN. Rotation in Red Giants. [Doctoral Dissertation]. The Ohio State University; 2018. Available from: http://rave.ohiolink.edu/etdc/view?acc_num=osu1531927526281553

University of Sydney

20. Li, Gang. Asteroseismology of gamma Doradus stars with Kepler .

Degree: 2020, University of Sydney

URL: http://hdl.handle.net/2123/23393

► Stellar physics is a vital part of modern astronomy. To better understand stars, we must understand not only the stellar surface, but also the stellar… (more)

Subjects/Keywords: Asteroseismology; stellar rotation; gamma Doradus stars; eclipsing binaries

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APA (6^th Edition):

Li, G. (2020). Asteroseismology of gamma Doradus stars with Kepler . (Thesis). University of Sydney. Retrieved from http://hdl.handle.net/2123/23393

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

Chicago Manual of Style (16^th Edition):

Li, Gang. “Asteroseismology of gamma Doradus stars with Kepler .” 2020. Thesis, University of Sydney. Accessed March 07, 2021. http://hdl.handle.net/2123/23393.

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

MLA Handbook (7^th Edition):

Li, Gang. “Asteroseismology of gamma Doradus stars with Kepler .” 2020. Web. 07 Mar 2021.

Vancouver:

Li G. Asteroseismology of gamma Doradus stars with Kepler . [Internet] [Thesis]. University of Sydney; 2020. [cited 2021 Mar 07]. Available from: http://hdl.handle.net/2123/23393.

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

Council of Science Editors:

Li G. Asteroseismology of gamma Doradus stars with Kepler . [Thesis]. University of Sydney; 2020. Available from: http://hdl.handle.net/2123/23393

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

21. Saulo Carneiro Maciel. Uma análise teórica da evolução da rotação estelar.

Degree: 2007, Universidade Federal do Rio Grande do Norte

URL: http://bdtd.bczm.ufrn.br/tedesimplificado//tde_busca/arquivo.php?codArquivo=1502

►

Nos últimos cinqüenta anos, grandes esforços foram feitos no intuito de se entender a evolução estelar. No contexto observacional, medidas precisas da velocidade rotacional projetada… (more)

▼

Nos últimos cinqüenta anos, grandes esforços foram feitos no intuito de se entender a evolução estelar. No contexto observacional, medidas precisas da velocidade rotacional projetada foram produzidas, em particular, pelos grupos de Natal e Genebra. Destes dados é possível no presente momento estabelecer o comportamento da rotação estelar do turnoﬀ até o ramo das gigantes vermelhas. Em adicional, estes dados têm mostrado o papel dos efeitos de marés na rotação estelar em sistemas binários próximos. Mesmo tendo sido feitos bons avanços c no ambito observacional, pouca atençã tem sido dada a estudos teóricos da evolução da rotação ao longo do diagrama HR, um tópico que está intimamente ligado a evolução das estrelas. Basicamente, existem dois motivos para tal fato,(i) a não suposição de simetria esférica leva a um aumento substancial da complexidade numérica das equações, e (ii) os modelos sem rotação têm tido bastante sucesso na explicação de relevantes dados observacionais, incluindo as relações entre massa e luminosidade e abundâncias químicas. Diante do avanço do estudo da rotação, ainda restam trabalhos a serem feitos sobre o seu papel em estágios mais tardios da evolução, uma vez que existem discordâncias entre predições teóricas e observacionais. No presente trabalho, nós estudamos o comportamento evolucionário da rotação ao longo do diagrama HR, levando em conta condições de contorno baseadas em recentes medidas de velocidade rotacional obtidas a partir de procedimentos de alta precisão e novos códigos evolutivos

In the past 50 years, large eﬀorts have been made toward the understanding of the stellar evolution. In the observational context, large sets of precise measurements of projected rotational velocity were produced, in particular by the Natal and Geneva groups. From these data, it is now possible to establish the behavior of stellar rotation from the turnoﬀ to the red giant branch. In addition, these data have shown the role of tidal eﬀects on stellar rotation in close binary systems. Nevertheless, relatively little attention has been paid to theoretical studies on the evolution of rotation along the HR Diagram, a topic itself directly associated to the evolution of the stars. Basically, there are two reasons for such a fact, (i) spherical symmetry is not assumed, what leads to a substantial increase in the numerical complexity of equations and (ii) non rotating models have been very successful in explaining relevant observational data, including the mass-luminosity relation and chemical abundances. In spite of these facts, it is clear that considerable work remains to be done on the role of rotation in the later stages of the evolution, where clear disagreements arise from confrontations between theoretical predictions and observations. In the present work we study the evolutionary behavior of stellar rotation along the HR Diagram, taking into account constraint conditions issued from recent observational survey of rotational velocity carried out with high precision…

Advisors/Committee Members: José Renan de Medeiros, José Dias do Nascimento Júnior, José Ronaldo Pereira da Silva.

Subjects/Keywords: Rotação; Estrelas subgigantes; Estrelas gigantes; Análise teórica; Subgiants stars; ASTRONOMIA ESPACIAL; Rotation; Giants stars; Theoretical analysis

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APA · Chicago · MLA · Vancouver · CSE | Export to Zotero / EndNote / Reference Manager

APA (6^th Edition):

Maciel, S. C. (2007). Uma análise teórica da evolução da rotação estelar. (Thesis). Universidade Federal do Rio Grande do Norte. Retrieved from http://bdtd.bczm.ufrn.br/tedesimplificado//tde_busca/arquivo.php?codArquivo=1502

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

Chicago Manual of Style (16^th Edition):

Maciel, Saulo Carneiro. “Uma análise teórica da evolução da rotação estelar.” 2007. Thesis, Universidade Federal do Rio Grande do Norte. Accessed March 07, 2021. http://bdtd.bczm.ufrn.br/tedesimplificado//tde_busca/arquivo.php?codArquivo=1502.

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

MLA Handbook (7^th Edition):

Maciel, Saulo Carneiro. “Uma análise teórica da evolução da rotação estelar.” 2007. Web. 07 Mar 2021.

Vancouver:

Maciel SC. Uma análise teórica da evolução da rotação estelar. [Internet] [Thesis]. Universidade Federal do Rio Grande do Norte; 2007. [cited 2021 Mar 07]. Available from: http://bdtd.bczm.ufrn.br/tedesimplificado//tde_busca/arquivo.php?codArquivo=1502.

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

Council of Science Editors:

Maciel SC. Uma análise teórica da evolução da rotação estelar. [Thesis]. Universidade Federal do Rio Grande do Norte; 2007. Available from: http://bdtd.bczm.ufrn.br/tedesimplificado//tde_busca/arquivo.php?codArquivo=1502

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

University of Exeter

22. Finley, A. Constraining the angular momentum-loss rates of the Sun and other Sun-like stars.

Degree: PhD, 2020, University of Exeter

URL: http://hdl.handle.net/10871/121115

► Stellar rotation, convection, and magnetism are intricately linked in low-mass stars like the Sun. In their outer convective envelopes, the interplay of rotation and convection… (more)

Subjects/Keywords: solar wind; stellar winds; astrophysics; magnetohydrodynamics; numerical simulation; rotation period evolution; low-mass stars; sun-like stars

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APA · Chicago · MLA · Vancouver · CSE | Export to Zotero / EndNote / Reference Manager

APA (6^th Edition):

Finley, A. (2020). Constraining the angular momentum-loss rates of the Sun and other Sun-like stars. (Doctoral Dissertation). University of Exeter. Retrieved from http://hdl.handle.net/10871/121115

Chicago Manual of Style (16^th Edition):

Finley, A. “Constraining the angular momentum-loss rates of the Sun and other Sun-like stars.” 2020. Doctoral Dissertation, University of Exeter. Accessed March 07, 2021. http://hdl.handle.net/10871/121115.

MLA Handbook (7^th Edition):

Finley, A. “Constraining the angular momentum-loss rates of the Sun and other Sun-like stars.” 2020. Web. 07 Mar 2021.

Vancouver:

Finley A. Constraining the angular momentum-loss rates of the Sun and other Sun-like stars. [Internet] [Doctoral dissertation]. University of Exeter; 2020. [cited 2021 Mar 07]. Available from: http://hdl.handle.net/10871/121115.

Council of Science Editors:

Finley A. Constraining the angular momentum-loss rates of the Sun and other Sun-like stars. [Doctoral Dissertation]. University of Exeter; 2020. Available from: http://hdl.handle.net/10871/121115

23. Patten, Brian Michael. The evolution of rotation and activity in young open clusters : the zero-age main sequence.

Degree: PhD, 2009, University of Hawaii – Manoa

URL: http://hdl.handle.net/10125/9356

►

Microfiche.

x, 112 leaves, bound ill. (some col.) 29 cm

I have undertaken a program of ground- and space-based observations to measure photometric rotation periods… (more)

▼

Microfiche.

x, 112 leaves, bound ill. (some col.) 29 cm

I have undertaken a program of ground- and space-based observations to measure photometric rotation periods and X-ray luminosities for late-type stars in the young open clusters IC 2391 and IC 2602. With cluster ages of ~30 Myr, IC 2391 and IC 2602 are ideal sites in which to observe conditions at the ZAMS since the solar-type stars in these clusters have not been on the main sequence long enough to undergo significant magnetic braking. The ROBAT survey of IC 2391 revealed 80 X-ray sources, 44 of which were found to be associated with stars which are now classified as new cluster members. Among the solar-type stars in both IC 2391 and IC 2602, I find a factor of ~25 spread in the distribution of rotation periods, which range from 0.21 to 4.86 day. I also find a factor of ~10-20 spread in the range of Lx about a median Lx value of ~10³⁰ erg S^-1 for both clusters. These results show conclusively that stars arrive on the ZAMS with a wide range of rotation rates and coronal activity levels. When compared to data from older clusters, such as the Pleiades and the Hyades, there is an overall decline observed in both the rotation rates and median X-ray luminosity of cluster members with increasing age, however, while the spread in the range of rotation rates decreases to a small value, the spread in the range of Lx values as a fraction of the median is observed to increase with age. This behavior is best explained through a dependence of Lx on Prot which is weak in the young clusters and strong in the older clusters. The Rossby diagram shows there is a tight correlation between Lx/ Lbol and the Rossby number, Prot divided by the convective turnover time. Young, rapidly rotating, main sequence stars lie along a plateau of magnetic saturation, where Lx has a weak dependence on rotation period, while older, more slowly rotating stars lie in a region on the Rossby diagram where Lx has a strong dependence on rotation period.

Subjects/Keywords: Cool stars – Luminosity function; Cool stars – Rotation

…for Ie 2602 Suspected Members........... 44 6 Rotation Data for Late-Type Stars in IC… …rotation rate and convective mixing rate. The braking of rotation in MS stars is therefore a… …measure rotation periods for solar-type stars in both clusters, and to measure coronal activity… …Chapter 3: Rotation at the ZAMS… …90 4.5 Long-Term Activity Cycles........................ 91 4.6 Lx versus Rotation…

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APA · Chicago · MLA · Vancouver · CSE | Export to Zotero / EndNote / Reference Manager

APA (6^th Edition):

Patten, B. M. (2009). The evolution of rotation and activity in young open clusters : the zero-age main sequence. (Doctoral Dissertation). University of Hawaii – Manoa. Retrieved from http://hdl.handle.net/10125/9356

Chicago Manual of Style (16^th Edition):

Patten, Brian Michael. “The evolution of rotation and activity in young open clusters : the zero-age main sequence.” 2009. Doctoral Dissertation, University of Hawaii – Manoa. Accessed March 07, 2021. http://hdl.handle.net/10125/9356.

MLA Handbook (7^th Edition):

Patten, Brian Michael. “The evolution of rotation and activity in young open clusters : the zero-age main sequence.” 2009. Web. 07 Mar 2021.

Vancouver:

Patten BM. The evolution of rotation and activity in young open clusters : the zero-age main sequence. [Internet] [Doctoral dissertation]. University of Hawaii – Manoa; 2009. [cited 2021 Mar 07]. Available from: http://hdl.handle.net/10125/9356.

Council of Science Editors:

Patten BM. The evolution of rotation and activity in young open clusters : the zero-age main sequence. [Doctoral Dissertation]. University of Hawaii – Manoa; 2009. Available from: http://hdl.handle.net/10125/9356

University of Arizona

24. Fleming, Thomas Anthony. Optical analysis of an x-ray selected sample of stars.

Degree: 1988, University of Arizona

URL: http://hdl.handle.net/10150/184366

► I analyse an x-ray selected sample of 128 late-type (F-M) stars. These stars were identified as optical counterparts to serendipitous x-ray detections made by the… (more)

▼ I analyse an x-ray selected sample of 128 late-type (F-M) stars. These stars were identified as optical counterparts to serendipitous x-ray detections made by the Einstein Observatory Extended Medium Sensitivity Survey. Once identified as x-ray sources, the stars were reobserved with an extensive program of optical observations consisting of high- and low-resolution spectroscopy and photometry. Spectral types, luminosity classes, absolute magnitudes, distances, x-ray luminosities, projected rotation rates (v sin i), radial velocities, and binary status have been determined for the sample. I find that Lₓ is correlated with v sin i for single stars. However, Lₓ does not correlate with Ω sin i, which leads me to believe that the correlation seen with v sin i is actually a correlation with radius. Indeed, Lₓ correlates strongly with radius (color, mass) for main sequence stars. This result provides a plausibility argument for rotational saturation in the coronae of late-type stars. Since this sample is flux limited, I use sky coverage and sensitivity information from the Einstein Observatory to calculate the bright end of the x-ray luminosity function for late-type stars. It appears that previously calculated luminosity functions from optically selected samples have underestimated the number of x-ray bright F and G dwarfs. I have also discovered 8 previously uncatalogued M dwarfs within 25 pc of the sun. My sample includes only M dwarfs of spectral type M5 and earlier, 93% of which are "emission" stars (i.e. type Me V), as well as two pre-main sequence M stars. Arguments involving kinematics and stellar rotational velocities are used to estimate the age of these x-ray "bright" M dwarfs; they appear to be quite young (≤ 1-3 x 10⁹ yrs). Since the local space density of x-ray "bright" M dwarfs increases with mass, I infer a longer activity timescale for lower masses. M dwarfs later than M5 lie below the sample's x-ray sensitivity limit. An upper limit of log Lₓ = 27.45 is put on their coronal emission. I also present H(α) and Ca II K line fluxes for most members of the M dwarf sample and show that the H(α) and Ca II K luminosities do indeed correlate with Lₓ. However, these chromospheric luminosities are weaker functions of rotation than Lₓ and may, in fact, represent saturated levels of activity. My results are consistent with the hypothesis that the chromosphere is heated by x-rays from the overlying corona. Finally, I discuss two unusual members of the sample which are attractive candidates for the recently proposed class of FK Comae stars. Advisors/Committee Members: Liebert, Jim (advisor).

Subjects/Keywords: X-ray astronomy.; Stars – Luminosity function.; Stars – Rotation.

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APA (6^th Edition):

Fleming, T. A. (1988). Optical analysis of an x-ray selected sample of stars. (Doctoral Dissertation). University of Arizona. Retrieved from http://hdl.handle.net/10150/184366

Chicago Manual of Style (16^th Edition):

Fleming, Thomas Anthony. “Optical analysis of an x-ray selected sample of stars. ” 1988. Doctoral Dissertation, University of Arizona. Accessed March 07, 2021. http://hdl.handle.net/10150/184366.

MLA Handbook (7^th Edition):

Fleming, Thomas Anthony. “Optical analysis of an x-ray selected sample of stars. ” 1988. Web. 07 Mar 2021.

Vancouver:

Fleming TA. Optical analysis of an x-ray selected sample of stars. [Internet] [Doctoral dissertation]. University of Arizona; 1988. [cited 2021 Mar 07]. Available from: http://hdl.handle.net/10150/184366.

Council of Science Editors:

Fleming TA. Optical analysis of an x-ray selected sample of stars. [Doctoral Dissertation]. University of Arizona; 1988. Available from: http://hdl.handle.net/10150/184366

25. Gagnier, Damien. Dynamique des étoiles massives proches de la rotation critique : Dynamics of massive stars at rotation rates close to criticality.

Degree: Docteur es, Astrophysique, Sciences de l'Espace, Planétologie, 2020, Université Toulouse III – Paul Sabatier

URL: http://www.theses.fr/2020TOU30159

►

La rotation joue un rôle majeur sur la dynamique, la structure et l'évolution séculaire des étoiles massives, souvent rotateurs rapides. Elle implique le mélange des… (more)

▼

La rotation joue un rôle majeur sur la dynamique, la structure et l'évolution séculaire des étoiles massives, souvent rotateurs rapides. Elle implique le mélange des éléments chimiques synthétisés dans leur cœur convectif, et la redistribution du moment cinétique dans leur enveloppe radiative. La rotation influence également le vent radiatif présent à leur surface, et modifie ainsi les pertes de masse et de moment cinétique associées. L'objectif de ce travail de thèse est multiple : nous cherchons à déterminer le rôle de la rotation sur les pertes de masse et de moment cinétique associées aux vents radiatifs des étoiles massives, comprendre le rôle de ces vents radiatifs sur leur évolution rotationnelle séculaire, et déterminer les implications d'une perte de moment cinétique sur la dynamique de l'enveloppe radiative de ces étoiles. Nous montrons que deux régimes de vent peuvent exister, l'un d'eux résulte en un fort flux de masse équatorial, donc en une forte perte de moment cinétique. Cette perte accrue de moment cinétique peut empêcher les étoiles massives d'atteindre une rotation critique avant la fin de la séquence principale. Enfin, l'étude du couplage entre les vents radiatifs et la dynamique de l'enveloppe radiative des étoiles massives en rotation montre que la couche de Stewartson est une caractéristique clé de l'écoulement pour le transport des éléments chimiques entre le cœur convectif et la surface des étoiles massives.

Rotation plays a major role in the dynamics, structure and secular evolution of, often rapidly rotating, massive stars. It leads to the mixing of chemical elements synthesised in their convective core, and to the transport of angular momentum in their radiative envelope. Rotation also influences the radiation-driven wind on their surface, and thus modifies the associated losses of mass and angular momentum. The objective of this thesis is multifold: we seek to determine the role of rotation on the mass and angular momentum losses associated with massive stars radiation-driven winds, to understand the role of such radiation-driven winds on their secular rotational evolution, and to determine the implications of a loss of angular momentum on the dynamics of the radiative envelope of these stars. We show that two different wind regimes can exist, one of them results in a strong equatorial mass flux, and thus in a high angular momentum loss rate. Such increased angular momentum loss may prevent massive stars from reaching critical rotation before the end of the main sequence. Regarding the coupling between radiative winds and the dynamics of the radiative envelope of massive rotating stars, we show that the Stewartson layer is a key component for the transport of chemical elements between the convective core and the surface of massive stars.

Advisors/Committee Members: Rieutord, Michel (thesis director), Charbonnel, Corinne (thesis director).

Subjects/Keywords: Étoiles massives; Rotation; Vents radiatifs; Dynamique des fluides astrophysiques; Massive stars; Rotation; Radiation-driven winds; Strophysical fluid dynamics

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APA (6^th Edition):

Gagnier, D. (2020). Dynamique des étoiles massives proches de la rotation critique : Dynamics of massive stars at rotation rates close to criticality. (Doctoral Dissertation). Université Toulouse III – Paul Sabatier. Retrieved from http://www.theses.fr/2020TOU30159

Chicago Manual of Style (16^th Edition):

Gagnier, Damien. “Dynamique des étoiles massives proches de la rotation critique : Dynamics of massive stars at rotation rates close to criticality.” 2020. Doctoral Dissertation, Université Toulouse III – Paul Sabatier. Accessed March 07, 2021. http://www.theses.fr/2020TOU30159.

MLA Handbook (7^th Edition):

Gagnier, Damien. “Dynamique des étoiles massives proches de la rotation critique : Dynamics of massive stars at rotation rates close to criticality.” 2020. Web. 07 Mar 2021.

Vancouver:

Gagnier D. Dynamique des étoiles massives proches de la rotation critique : Dynamics of massive stars at rotation rates close to criticality. [Internet] [Doctoral dissertation]. Université Toulouse III – Paul Sabatier; 2020. [cited 2021 Mar 07]. Available from: http://www.theses.fr/2020TOU30159.

Council of Science Editors:

Gagnier D. Dynamique des étoiles massives proches de la rotation critique : Dynamics of massive stars at rotation rates close to criticality. [Doctoral Dissertation]. Université Toulouse III – Paul Sabatier; 2020. Available from: http://www.theses.fr/2020TOU30159

26. Evano, Benjamin. Analyse semiclassique des modes d'oscillation chaotiques dans les étoiles en rotation rapide : Semiclassical analysis of chaotic oscillation modes in rapidly rotating stars.

Degree: Docteur es, Astrophysique, sciences de l'espace, planétologie, 2019, Université Toulouse III – Paul Sabatier

URL: http://www.theses.fr/2019TOU30173

►

L'astérosismologie permet d'obtenir des informations sur la structure interne des étoiles par l'étude de leurs pulsations. Parmi les cibles des satellites CoRot, Kepler ou Tess,… (more)

▼

L'astérosismologie permet d'obtenir des informations sur la structure interne des étoiles par l'étude de leurs pulsations. Parmi les cibles des satellites CoRot, Kepler ou Tess, il y a une part importante d'étoiles en rotation rapide dont le spectre est encore difficile à exploiter. La mauvaise compréhension de la structure du spectre est l'une des raisons de cette difficulté. Les méthodes asymptotiques sont efficaces pour comprendre l'organisation du spectre et la relier aux propriétés physiques de l'étoile. Asymptotiquement, la propagation des rayons acoustiques est décrite par un système Hamiltonien. Si l'étoile est quasi sphérique, la dynamique du système est complètement intégrable. Toutefois, la rotation aplatit l'étoile, ce qui entraîne une transition de la dynamique vers un régime mixte avec à la fois des zones intégrables et des zones chaotiques dans l'espace des phases. Dans cette thèse nous étudions les modes propres d'oscillation associés aux régions chaotiques de l'espace des phases. Les modes chaotiques usuellement étudiés, e.g. dans les billards quantiques ou les cavités optiques, ont un spectre irrégulier qui suit une distribution statistique prédite par la théorie des matrices aléatoires. Les étoiles se distinguent de ces systèmes par le fait que le milieux stellaire est fortement inhomogène. En particulier la vitesse du son est plus faible en surface de plusieurs ordres de grandeurs par rapport au cœur. Ainsi, le temps de parcours entre deux rebonds est approximativement le même pour tous les rayons acoustiques. En utilisant les outils du chaos quantique, nous montrons que cet effet provoque un espacement régulier des fréquences dans le spectre des modes chaotiques, que l'on peut relier à une moyenne de la vitesse du son dans l'intérieur stellaire. Ce résultat permet de mieux comprendre la structure asymptotique du spectre des modes de pression dans les étoiles en rotation rapide.

Asteroseismology provides information on the internal structure of stars by studying their pulsations. Among the targets of CoRot, Kepler or Tess satellites, there is an important part of rapidly rotating stars whose spectrum is still difficult to exploit. The poor understanding of the spectrum structure is one of the reasons for this difficulty. Asymptotic methods are effective to understand the organization of the spectrum and relate it to the physical properties of the star. Asymptotically, the propagation of acoustic rays is described by a Hamiltonian system. If the star is almost spherical, the dynamics of the system is completely integrable. However, the rotation flattens the star, resulting in a transition of the dynamics to a mixed regime with both integrable zones and chaotic zones in the phase space. In this thesis we study the oscillation modes associated with chaotic regions of phase space. The chaotic modes usually studied, e.g. in quantum billiards or optical cavities, have an irregular spectrum which follows a statistical distribution predicted by Random Matrix Theory. Stars differ from these systems by…

Advisors/Committee Members: Lignières, François (thesis director), Georgeot, Bertrand (thesis director).

Subjects/Keywords: Étoiles en rotation; Ondes; Chaos classique; Chaos quantiques; Waves; Rotating stars; Classical chaos; Quantum chaos

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APA (6^th Edition):

Evano, B. (2019). Analyse semiclassique des modes d'oscillation chaotiques dans les étoiles en rotation rapide : Semiclassical analysis of chaotic oscillation modes in rapidly rotating stars. (Doctoral Dissertation). Université Toulouse III – Paul Sabatier. Retrieved from http://www.theses.fr/2019TOU30173

Chicago Manual of Style (16^th Edition):

Evano, Benjamin. “Analyse semiclassique des modes d'oscillation chaotiques dans les étoiles en rotation rapide : Semiclassical analysis of chaotic oscillation modes in rapidly rotating stars.” 2019. Doctoral Dissertation, Université Toulouse III – Paul Sabatier. Accessed March 07, 2021. http://www.theses.fr/2019TOU30173.

MLA Handbook (7^th Edition):

Evano, Benjamin. “Analyse semiclassique des modes d'oscillation chaotiques dans les étoiles en rotation rapide : Semiclassical analysis of chaotic oscillation modes in rapidly rotating stars.” 2019. Web. 07 Mar 2021.

Vancouver:

Evano B. Analyse semiclassique des modes d'oscillation chaotiques dans les étoiles en rotation rapide : Semiclassical analysis of chaotic oscillation modes in rapidly rotating stars. [Internet] [Doctoral dissertation]. Université Toulouse III – Paul Sabatier; 2019. [cited 2021 Mar 07]. Available from: http://www.theses.fr/2019TOU30173.

Council of Science Editors:

Evano B. Analyse semiclassique des modes d'oscillation chaotiques dans les étoiles en rotation rapide : Semiclassical analysis of chaotic oscillation modes in rapidly rotating stars. [Doctoral Dissertation]. Université Toulouse III – Paul Sabatier; 2019. Available from: http://www.theses.fr/2019TOU30173

University of Pennsylvania

27. Gilhool, Steven. Spectroscopic Analysis Of Stellar Rotational Velocity At The Bottom Of The Main Sequence.

Degree: 2018, University of Pennsylvania

URL: https://repository.upenn.edu/edissertations/3043

► This thesis presents analyses aimed at understanding the rotational properties of stars at the bottom of the main sequence. The evolution of stellar angular momentum… (more)

▼ This thesis presents analyses aimed at understanding the rotational properties of stars at the bottom of the main sequence. The evolution of stellar angular momentum is intertwined with magnetic field generation, mass outflows, convective motions, and many other stellar properties and processes. This complex interplay has made a comprehensive understanding of stellar angular momentum evolution elusive. This is particularly true for low-mass stars due to the observational challenges they present. At the very bottom of the main sequence (spectral type < M4), stars become fully convective. While this ‘Transition to Complete Convection’ presents mysteries of its own, observing the rotation of stars across this boundary can provide insight into stellar structure and magnetic fields, as well as their role in driving the evolution of stellar angular momentum. I present here a review of our understanding of rotational evolution in stars of roughly solar mass down to the end of the main sequence. I detail our efforts to determine large numbers of rotational velocity measurements for M dwarfs observed by the Apache Point Galactic Evolution Experiment (APOGEE). We analyzed the 714 M dwarfs as late as spectral type ~ M7, the largest sample of M dwarfs to date. Consistent with the hypothesis that fully-convective M dwarfs spin down more slowly than solar-type stars, we found that the fraction of detectably rotating stars jumped from about 10% for early to mid M dwarfs, to about 35% for late M dwarfs. We also found some interesting tension between the rotation fractions from spectroscopic studies of vsini like ours, and those expected from rotation periods derived from photometric surveys. Finally, I describe our novel data-driven technique for rapidly estimating vsini in survey data. Rather than directly measuring the broadening of spectral lines, we leveraged the large information content of high-resolution spectral data to empirically estimate vsini. This computationally efficient technique provides a means of rapidly estimating vsini for large numbers of stars in spectroscopic survey data. Indeed, we were able to estimate vsini up to 15 km s-1 for 27,000 APOGEE spectra, in fractions of a second per spectrum.

Subjects/Keywords: data analysis; infrared; low-mass stars; rotation; spectroscopy; statistics; Astrophysics and Astronomy

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APA · Chicago · MLA · Vancouver · CSE | Export to Zotero / EndNote / Reference Manager

APA (6^th Edition):

Gilhool, S. (2018). Spectroscopic Analysis Of Stellar Rotational Velocity At The Bottom Of The Main Sequence. (Thesis). University of Pennsylvania. Retrieved from https://repository.upenn.edu/edissertations/3043

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

Chicago Manual of Style (16^th Edition):

Gilhool, Steven. “Spectroscopic Analysis Of Stellar Rotational Velocity At The Bottom Of The Main Sequence.” 2018. Thesis, University of Pennsylvania. Accessed March 07, 2021. https://repository.upenn.edu/edissertations/3043.

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

MLA Handbook (7^th Edition):

Gilhool, Steven. “Spectroscopic Analysis Of Stellar Rotational Velocity At The Bottom Of The Main Sequence.” 2018. Web. 07 Mar 2021.

Vancouver:

Gilhool S. Spectroscopic Analysis Of Stellar Rotational Velocity At The Bottom Of The Main Sequence. [Internet] [Thesis]. University of Pennsylvania; 2018. [cited 2021 Mar 07]. Available from: https://repository.upenn.edu/edissertations/3043.

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

Council of Science Editors:

Gilhool S. Spectroscopic Analysis Of Stellar Rotational Velocity At The Bottom Of The Main Sequence. [Thesis]. University of Pennsylvania; 2018. Available from: https://repository.upenn.edu/edissertations/3043

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

28. Karageorgopoulos, Vasileios. Υπολογιστική σχετικιστική μελέτη των αστέρων νετρονίων με γενίκευση της μεθόδου των μετανευτώνειων προσεγγίσεων.

Degree: 2017, University of Patras; Πανεπιστήμιο Πατρών

URL: http://hdl.handle.net/10442/hedi/40229

► The main subject of the present PhD Thesis is the rotating relativistic polytropic models of neutron stars. The final purpose is to compute the physical… (more)

▼ The main subject of the present PhD Thesis is the rotating relativistic polytropic models of neutron stars. The final purpose is to compute the physical characteristics of a neutron star in case of hydrostatic equillibrium, of uniform rotation with further study regarding in differential rotation, as well as in case of a neutron star embbeded in a chameleon scalar field. In order to study these problems we have to solve Einstein's equations. Because of the nonlinearity of Einstein's equations, there are not exact solutions describing motions of such objects. So, we adopt the “post-Newtonian approximation” (PNA) scheme, which is a perdurbative approximative scheme for solving Einstein's equations. Post-Newtonian expansions in general relativity are used for finding an approximate solution of the Einstein field equations for the metric tensor. As any approximation scheme, requires some small parameters characterizing the nature of the system under consideration. The post-Newtonian approximation is expanded in small parameters which express orders of deviations from Newton's law of universal gravitation. Typical parameters are the so-called relativistic parameter represents the relativistic behaviour of the system under consideration, and the so-called rotation parameter represents the distortion due to rotation. The post-Newtonian approximation scheme gives Newtonian description in the lowest order and general relativistic effects as higher order perturbations. There are many astrophysical systems where Newtonian gravity is dominant, but general relativistic gravity plays also an important role in their evolution. The present PhD Thesis consistis of six Chapters. In Chapter 1, we discuss the background physics regarding neutron stars. In Chapter 2, we describe the structure of neutron stars and present the various equations of states used for numerical comptutations. In the final part of this chapter, we develope and apply a parallel code for solving with multiprecision (of 32 digits) the problem of the undistorted polytropic model. In Chapter 3, present the theoritical background of relativistic polytropic models within the framework of PNA and the numerical method developed and used in our computations. In Chapter 4, we revisit the problem of computing uniformly rotating polytropic models by using PNA and we solve the problem in complex plane using the so-called “complex plane strategy” (CPS). We achieve to remove certain difficulties, otherwise involved in the computations of general – relativistic polytropic models simulating rapidly rotating neutron stars, and to compute results of improved accuracy when compared to corresponding results of other reliable numerical methods. In order to expand our study to fully relativistic polytropic models and compute general-relativistic polytropic models in critical rigid rotation, we develop a “hybrid approximative scheme” (HAS), in the framework of the post-Newtonian approximation (Chapter 5). We treat the differential equations governing such a model as a “complex initial…

Subjects/Keywords: Αστέρες νετρονίων; Σχετικιστικά πολυτροπικά μοντέλα; Μετανευτώνειες προσεγγίσεις; Κρίσιμη περιστροφή; Ομοιόμορφη περιστροφή; ΔΙΑΦΟΡΙΚΗ ΠΕΡΙΣΤΡΟΦΗ; Αστέρες χαμαιλέοντες; Διαταρακτικές μέθοδοι; Στρατηγική του μιγαδικού επιπέδου; Neutron stars; General-relativistic polytropic models; Post-Newtonian approximation; Critical rotation; Uniform rotation; DIFFERENTIAL ROTATION; Chameleon stars; Perturbation methods; Complex plane strategy

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APA · Chicago · MLA · Vancouver · CSE | Export to Zotero / EndNote / Reference Manager

APA (6^th Edition):

Karageorgopoulos, V. (2017). Υπολογιστική σχετικιστική μελέτη των αστέρων νετρονίων με γενίκευση της μεθόδου των μετανευτώνειων προσεγγίσεων. (Thesis). University of Patras; Πανεπιστήμιο Πατρών. Retrieved from http://hdl.handle.net/10442/hedi/40229

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

Chicago Manual of Style (16^th Edition):

Karageorgopoulos, Vasileios. “Υπολογιστική σχετικιστική μελέτη των αστέρων νετρονίων με γενίκευση της μεθόδου των μετανευτώνειων προσεγγίσεων.” 2017. Thesis, University of Patras; Πανεπιστήμιο Πατρών. Accessed March 07, 2021. http://hdl.handle.net/10442/hedi/40229.

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

MLA Handbook (7^th Edition):

Karageorgopoulos, Vasileios. “Υπολογιστική σχετικιστική μελέτη των αστέρων νετρονίων με γενίκευση της μεθόδου των μετανευτώνειων προσεγγίσεων.” 2017. Web. 07 Mar 2021.

Vancouver:

Karageorgopoulos V. Υπολογιστική σχετικιστική μελέτη των αστέρων νετρονίων με γενίκευση της μεθόδου των μετανευτώνειων προσεγγίσεων. [Internet] [Thesis]. University of Patras; Πανεπιστήμιο Πατρών; 2017. [cited 2021 Mar 07]. Available from: http://hdl.handle.net/10442/hedi/40229.

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

Council of Science Editors:

Karageorgopoulos V. Υπολογιστική σχετικιστική μελέτη των αστέρων νετρονίων με γενίκευση της μεθόδου των μετανευτώνειων προσεγγίσεων. [Thesis]. University of Patras; Πανεπιστήμιο Πατρών; 2017. Available from: http://hdl.handle.net/10442/hedi/40229

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

Université de Montréal

29. Van Grootel, Valérie. Étude des étoiles de la branche horizontale extrême par l'astérosismologie.

Degree: 2008, Université de Montréal

URL: http://hdl.handle.net/1866/6415

Subjects/Keywords: Étoiles; Stars; Oscillations-Étoiles; Oscillations-Stars; Intérieurs-Étoiles; Interior-Stars; Sous-naines-Étoiles; Subdwarfs-Stars; Branche horizentale extrême-Étoiles; Extreme horizental branch-Stars; Binaires; Binaries; Serrées-Étoiles; Close-Stars; Rotation-Étoiles; Rotation-Stars; Évolution; Evolution

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APA · Chicago · MLA · Vancouver · CSE | Export to Zotero / EndNote / Reference Manager

APA (6^th Edition):

Van Grootel, V. (2008). Étude des étoiles de la branche horizontale extrême par l'astérosismologie. (Thesis). Université de Montréal. Retrieved from http://hdl.handle.net/1866/6415

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

Chicago Manual of Style (16^th Edition):

Van Grootel, Valérie. “Étude des étoiles de la branche horizontale extrême par l'astérosismologie.” 2008. Thesis, Université de Montréal. Accessed March 07, 2021. http://hdl.handle.net/1866/6415.

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

MLA Handbook (7^th Edition):

Van Grootel, Valérie. “Étude des étoiles de la branche horizontale extrême par l'astérosismologie.” 2008. Web. 07 Mar 2021.

Vancouver:

Van Grootel V. Étude des étoiles de la branche horizontale extrême par l'astérosismologie. [Internet] [Thesis]. Université de Montréal; 2008. [cited 2021 Mar 07]. Available from: http://hdl.handle.net/1866/6415.

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

Council of Science Editors:

Van Grootel V. Étude des étoiles de la branche horizontale extrême par l'astérosismologie. [Thesis]. Université de Montréal; 2008. Available from: http://hdl.handle.net/1866/6415

Note: this citation may be lacking information needed for this citation format:
Not specified: Masters Thesis or Doctoral Dissertation

30. Jones, Jeremy W. The Ages of A-Stars.

Degree: PhD, Physics and Astronomy, 2016, Georgia State University

URL: https://scholarworks.gsu.edu/phy_astr_diss/86

► Stars with spectral type `A' (also called A-type stars or just A-stars) are bright intermediate mass stars (∼1.5-2.5 M_⊙) that make up ∼1% of… (more)

Subjects/Keywords: Astronomy; stars: early-type; stars: evolution; stars: rotation; stars: fundamental parameters; techniques: interferometric

…Spectral Type: Our Brightest Stellar Neighbors . . . 1 1.1.1 The Rapid Rotation of A-Stars… …stars with masses ranging from 1.0 to 2.5 M and an angular rotation rate of either 0% (… …The Rapid Rotation of A-Stars In addition to being more luminous than stars like our Sun, A… …the stellar wind to slow down rotation (Matt et al. 2012, 2015). A-stars, being… …interactions from these close companions could be the cause of their slow rotation. Ap stars, on the…

1 more image…

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APA · Chicago · MLA · Vancouver · CSE | Export to Zotero / EndNote / Reference Manager

APA (6^th Edition):

Jones, J. W. (2016). The Ages of A-Stars. (Doctoral Dissertation). Georgia State University. Retrieved from https://scholarworks.gsu.edu/phy_astr_diss/86

Chicago Manual of Style (16^th Edition):

Jones, Jeremy W. “The Ages of A-Stars.” 2016. Doctoral Dissertation, Georgia State University. Accessed March 07, 2021. https://scholarworks.gsu.edu/phy_astr_diss/86.

MLA Handbook (7^th Edition):

Jones, Jeremy W. “The Ages of A-Stars.” 2016. Web. 07 Mar 2021.

Vancouver:

Jones JW. The Ages of A-Stars. [Internet] [Doctoral dissertation]. Georgia State University; 2016. [cited 2021 Mar 07]. Available from: https://scholarworks.gsu.edu/phy_astr_diss/86.

Council of Science Editors:

Jones JW. The Ages of A-Stars. [Doctoral Dissertation]. Georgia State University; 2016. Available from: https://scholarworks.gsu.edu/phy_astr_diss/86

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Open Access Theses and Dissertations