Issue |
A&A
Volume 373, Number 1, July I 2001
|
|
---|---|---|
Page(s) | 190 - 198 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20010585 | |
Published online | 15 July 2001 |
Formation of massive stars by growing accretion rate*
Geneva Observatory, 1290 Sauverny, Switzerland e-mail: andre.maeder@obs.unige.ch
Corresponding author: R. Behrend, raoul.behrend@obs.unige.ch
Received:
3
April
2001
Accepted:
12
April
2001
We perform calculations of pre-main sequence evolution
of stars from 1 to with growing accretion rates
. The values of
are taken equal to a constant fraction
of the rates of
the mass outflows observed by Churchwell ([CITE]) and Henning
([CITE]). The evolution of the various stellar parameters is
given, as well as the evolution of the disc luminosity;
electronic tables are provided as a supplement to the articles. Typically, the
duration of the accretion phase of massive stars is
and there is less than
difference in the time necessary to form a 8 or
star.
If in a young cluster all the proto-stellar cores start to
accrete at the same time, we then have a relation
between the masses of the new stars and the time t of their
appearance. Since we also know the distribution of stellar masses at the end of star
formation (IMF), we can derive the star formation history
. Interestingly enough, the current IMF implies two
peaks of star formation: low mass stars form first and high mass
star form later.
Key words: stars: formation / stars: evolution / stars: pre-main sequence / stars: statistics / accretion, accretion discs / Hertzsprung-Russel (HR) and C / M diagrams
© ESO, 2001
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