Volume 373, Number 1, July I 2001
|Page(s)||190 - 198|
|Section||Interstellar and circumstellar matter|
|Published online||15 July 2001|
Formation of massive stars by growing accretion rate*
Geneva Observatory, 1290 Sauverny, Switzerland e-mail: firstname.lastname@example.org
Corresponding author: R. Behrend, email@example.com
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
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.