On the formation of the most massive stars in the galaxy
The most massive stars in the galaxy - those with more than 15 to 20 solar masses - are lilkely to ionize their surroundings before they reach their final mass. How can they accrete in spite of the presence of over-pressurized gas? This thesis presents results of Submillimeter Array (SMA) and Very L...
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| Главный автор: | |
|---|---|
| Формат: | Livre numérique |
| Язык: | Anglais |
| Опубликовано: |
New York, NY :
Springer New York
[20..].
Cham : Springer Nature |
| Редактирование: | 1st ed. 2012. |
| Серии: | Springer Theses, Recognizing Outstanding Ph.D. Research
|
| Online-ссылка: | Accès sur la plateforme de l'éditeur Accès sur la plateforme Istex Accès Université d'Orléans Accès INSA CVL |
| Примечание: |
Archives Springer e-books (Licence nationale) Archives Springer e-books (Licence nationale) |
| Autres localisations: | Voir dans le Sudoc |
| Edition sous un autre format: | • On the Formation of the Most Massive Stars in the Galaxy, doctoral thesis accepted by Universidad Nacional Autónoma de México, Roberto J. Galván-Madrid, New York, Springer, 2012, 1 vol. (XIII-122 p.), Springer theses, 978-1-4614-3307-1 • On the Formation of the Most Massive Stars in the Galaxy, Texte imprimé, 9781461433095 • On the Formation of the Most Massive Stars in the Galaxy, doctoral thesis accepted by Universidad Nacional Autónoma de México, Roberto J. Galván-Madrid, New York, Springer, 2012, 1 vol. (XIII-122 p.), Springer theses, 978-1-4614-3307-1 |
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| 100 | 1 | |a Galván-Madrid, Roberto J. | |
| 245 | 1 | 0 | |a On the formation of the most massive stars in the galaxy |c by Roberto J. Galván-Madrid. |
| 250 | |a 1st ed. 2012. | ||
| 260 | |a New York, NY : |b Springer New York. | ||
| 260 | |a Cham : |b Springer Nature, |c [20..]. | ||
| 490 | 0 | |a Springer Theses, Recognizing Outstanding Ph.D. Research |x 2190-5061 | |
| 500 | |a Archives Springer e-books (Licence nationale) | ||
| 500 | |a Archives Springer e-books (Licence nationale) | ||
| 505 | 1 | |a Foreword by Prof. Luis F. Rodriguez (CRyA-UNAM) and Dr. Qizhou Zhang (Harvard-Smithsonian Center for Astrophysics).-Chapter 1: Introduction to the Scientific Problem Chapter 2: A MSFR at the Onset of Ionization: W33A Chapter 3: A MSFR with young UC and HC HII Regions: G20.08N Chapter 4: Time Variability of HII Regions: A Signature of Accretion? Chapter 5: Time Variability of HII Regions in Numerical Simulations of MSFR Chapter 6: Conclusions Bibliography Appendix I: Radio and (Sub)millimeter Interferometers Appendix II: Molecular-line Emission Appendix III: Ionized-Gas Emission Index | |
| 506 | |a Accès en ligne pour les établissements français bénéficiaires des licences nationales | ||
| 506 | |a Accès soumis à abonnement pour tout autre établissement | ||
| 506 | |a Conditions particulières de réutilisation pour les bénéficiaires des licences nationales. https://www.licencesnationales.fr/springer-nature-ebooks-contrat-licence-ln-2017 | ||
| 520 | |a The most massive stars in the galaxy - those with more than 15 to 20 solar masses - are lilkely to ionize their surroundings before they reach their final mass. How can they accrete in spite of the presence of over-pressurized gas? This thesis presents results of Submillimeter Array (SMA) and Very Large Array (VLA) studies of massive star formation regions in the early stages of ionization, as well as an analysis of numerical simulations of the evolution of these young HII regions. The results favor a picture in which very massive stars form in accretion flows that are partially ionized and that keep accreting material from their environment.The American Astronomical Society selected Roberto Galvan-Madrid as a prize winner for The Rodger Doxsey Travel Prize in 2010 | ||
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