EPoS Contribution
EPoS Contribution
Protostellar Evolution and Massive Star Formation

Takashi Hosokawa
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, USA
massive star formation. In this contribution, I present our recent work on numerical modeling of massive protostars. First, I show evolution of massive protostars accreting at the rates of > 10^{-4} M_sun/yr. I explain that massive protostars have characteristic features, for example, very large radius exceeding 100 R_sun. Various aspects of evolution of massive protostars, including dependence on accretion geometry (spherical v.s. disk accretion), and implications for observations are also discussed. Next, I show evolution of massive pre-main-sequence (PMS) stars after mass accretion is shut off. Our calculations show that massive PMS stars approaches the zero-age main-sequence (ZAMS) stage over 10^{4-5} yr. I discuss the population and future detectability of such massive PMS stars.
Caption: Evolution tracks of massive pre-main-sequence stars in HR diagram. The solid curves represent the tracks of 10, 15, 20, and 25 M_sun stars. The symbols on the tracks indicate the elapsed time after mass accretion is shut off. The dotted line is the birth line with the accretion rate of 10^{-3} M_sun/yr, and the dashed line is the zero-age main-sequence line.
Collaborators:
T. J. Harries, Exeter, UK
D. A. Rundle, Exeter, UK
Key publication

Suggested Session: Early Phases of Disks