Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009apj...707.1438s&link_type=abstract
The Astrophysical Journal, Volume 707, Issue 2, pp. 1438-1448 (2009).
Astronomy and Astrophysics
Astronomy
3
Accretion, Accretion Disks, Dust, Extinction, Infrared: Stars, Radiative Transfer, Stars: Formation, Stars: Luminosity Function, Mass Function, Stars: Pre-Main Sequence
Scientific paper
Most early radiative transfer calculations of protostellar collapse have suggested an upper limit of ~40 M sun for the final stellar mass before radiation pressure can exceed the star's gravitational pull and halt the accretion. Here we perform further collapse calculations, using frequency-dependent radiation transfer coupled to a frequency-dependent dust model that includes amorphous carbon particles, silicates, and ice-coated silicates. The models start from pressure-bounded, logatropic spheres of mass between 5 M sun and 150 M sun with an initial nonsingular density profile. We find that in a logatrope the infall is never reversed by the radiative forces on the dust and that stars with masses gsim100 M sun may form by continued accretion. Compared to previous models that start the collapse with a ρ vprop r -2 density configuration, our calculations result in higher accretion times and lower average accretion rates with peak values of ~5.8 × 10-5 M sun yr-1. The radii and bolometric luminosities of the produced massive stars (gsim90 M sun) are in good agreement with the figures reported for detected stars with initial masses in excess of 100 M sun. The spectral energy distribution from the stellar photosphere reproduces the observed fluxes for hot molecular cores with peaks of emission from mid- to near-infrared.
Daza-Montero Judith
de Felice Fernando
Di Sigalotti Leonardo G.
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