Evidence for Disks around Young Massive Stars from 3D Radiative Transfer Image Modeling
HURÉ, J.-M.
Observatoire aquitain des sciences de l'univers [OASU]
Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
Laboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
Université Sciences et Technologies - Bordeaux 1 [UB]
Observatoire aquitain des sciences de l'univers [OASU]
Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
Laboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
Université Sciences et Technologies - Bordeaux 1 [UB]
SEMENOV, D.
A.N. Severtsov Institute of Ecology and Evolution
Max-Planck-Institut für Astronomie [MPIA]
< Reduce
A.N. Severtsov Institute of Ecology and Evolution
Max-Planck-Institut für Astronomie [MPIA]
Language
en
Communication dans un congrès
This item was published in
2007-09-14, Heidelberg. 2008, vol. 387, p. 270
English Abstract
While a paradigm for the formation of low-mass stars has been established that is based on accretion of gas and dust through a circumstellar disk, there is no agreed formation scenario for stars with masses greater than ...Read more >
While a paradigm for the formation of low-mass stars has been established that is based on accretion of gas and dust through a circumstellar disk, there is no agreed formation scenario for stars with masses greater than 10 solar masses. New evidence for the existence of large-scale flattened structures around young massive stars and compact H II regions is presented and analyzed by radiative transfer models: i) An analysis of the most-extended circumstellar disk known so far including a stability analysis of extended disk structures. ii) A comparison of K-band images of the first hypercompact H II region with a disk candidate and scattered light models. iii) A modeling of the first candidate for a remnant disk around a massive star.Read less <
Origin
Hal imported