Poster Talk abstract details
Radiative Magneto-Hydrodynamics in prestellar core collapse towards massive star formation
Abstract
A 1D-spherical cloud collapse to form a massive star is eventually stopped by the radiation pressure of the new born star. A disk structure with cavities (Krumholz, Klein & McKee (2005)) and a massive accretion disk (Yorke & Sonnhalter (2002) and Krumholz (2007)) is essential to transport sufficient material onto the star beyond the 1D radiation pressure limit.
Yet, even the 2D simulations indicate a low efficiency, e.g. very massive disks (120Msol) are needed to form a 43Msol star.
In our project we determine the effects of dimensionality (3D vs. 2D), combined with physical effects, e.g. radiation pressure, magnetic fields and self-gravity on the accretion rate as a function of disk mass and primary mass/luminosity. For that purpose we have developed a 3D-magneto-hydrodynamical code, including self-gravity, Flux-Limited Diffusion of radiation combined with ray-tracing irradiation.
Here we present our first simulation results and the current state of the project.
Please pay also attention to the collaborative project by Mario Flock (Radiative Hydrodynamics in circumstellar disks).
Yet, even the 2D simulations indicate a low efficiency, e.g. very massive disks (120Msol) are needed to form a 43Msol star.
In our project we determine the effects of dimensionality (3D vs. 2D), combined with physical effects, e.g. radiation pressure, magnetic fields and self-gravity on the accretion rate as a function of disk mass and primary mass/luminosity. For that purpose we have developed a 3D-magneto-hydrodynamical code, including self-gravity, Flux-Limited Diffusion of radiation combined with ray-tracing irradiation.
Here we present our first simulation results and the current state of the project.
Please pay also attention to the collaborative project by Mario Flock (Radiative Hydrodynamics in circumstellar disks).