Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aspc..267..165y&link_type=abstract
Hot Star Workshop III: The Earliest Stages of Massive Star Birth. ASP Conference Proceedings, Vol. 267. Edited by Paul A. Crowth
Astronomy and Astrophysics
Astronomy
15
Scientific paper
Radiative effects strongly hinder the formation of massive stars via accretion. A necessary condition for accretion growth of a hydrostatic object up to high masses M > 20 Msun (rather than coalescence of optically thick objects) is the formation of and accretion through a circumstellar disk. These disks will be photoevaporated on a timescale of 105 yr, similar to the accretion timescale, and be observed as UCHII's. Collapse simulations with grey radiation transfer display significantly different results from corresponding frequency-dependent simulations. A single example of a 60 Msun molecular core with resulting stellar masses of Mfinalgrey = 20.7 Msun and Mfinalnu = 33.6 Msun is briefly discussed. In order to include the effects of accretion in modifying the central source's luminosity evolution, a semi-analytical scheme for augmenting existing evolutionary tracks of pre-main sequence protostars is introduced and discussed. It is shown that the ``birthline'', i.e. the equilibrium position of fully convective, deuterium-burning stars in the HR diagram with cosmic deuterium abundance, is - strictly speaking - unattainable via accretion for stars more massive than 1 Msun.
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