On the formation of the most massive stars in the galaxy
General Material Designation
[Book]
First Statement of Responsibility
Roberto J. Galván-Madrid
.PUBLICATION, DISTRIBUTION, ETC
Place of Publication, Distribution, etc.
New York :
Name of Publisher, Distributor, etc.
Springer,
Date of Publication, Distribution, etc.
c2012
PHYSICAL DESCRIPTION
Specific Material Designation and Extent of Item
1 online resource (xiii, 122 p.) :
Other Physical Details
ill. (some col.)
SERIES
Series Title
Springer theses,
ISSN of Series
2190-5053
GENERAL NOTES
Text of Note
"Doctoral Thesis accepted by Universidad Nacional Autónoma de México."
INTERNAL BIBLIOGRAPHIES/INDEXES NOTE
Text of Note
Includes bibliographical references
SUMMARY OR ABSTRACT
Text of Note
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
OTHER EDITION IN ANOTHER MEDIUM
Title
On the formation of the most massive stars in the galaxy.