2012/09/09 by Patrick Hennebelle, Hennebelle, Patrick, Benoit Commercon +1
Physics and Astronomy · #Astrophysics of Galaxies (astro-ph.GA) #FOS: Physical sciences #Solar and Stellar Astrophysics (astro-ph.SR) #astro-ph.GA #astro-ph.SR
paper · pdf · doi:10.48550/arxiv.1209.1786
to appear in The Labyrinth of Star Formation, (eds.) D. Stamatellos, S. Goodwin, and D. Ward-Thompson, Springer
arxiv created 2012/09/09 · arxiv updated 2012/09/11
We briefly review the recent numerical works that have been performed to understand the formation of massive stars. After a brief description of the classical works, we review more specifically i) the problem of building stars more massive than 20 M_\odot and ii) how to prevent the massive cores to fragment in many objects. Multi-D simulations succeed in circumventing the radiative pressure leading to the formation of massive stars although some questions are still debated regarding how is accretion exactly proceeding. While the core fragmentation is slightly reduced by the radiative feedback and the magnetic field when they are treated separately, it is almost entirely suppressed when both of them are included. This is because, magnetic field by removing angular momentum focusses the flow in a compact region. This makes the radiative feedback very efficient leading to a significant increase of the temperature.