Modeling Accretion Disk Formation In Binary Systems

Details Modeling Accretion Disk Formation In Binary Systems Modeling Accretion Disk Formation In Binary Systems

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21940406h&link_type=abstract

American Astronomical Society, AAS Meeting #219, #404.06

Astronomy and Astrophysics

Astronomy

Scientific paper

We present new results of 3-D Adaptive Mesh Refinement (AMR) simulations exploring the evolution of accretion disks formed via wind capture in binary systems. Accretion onto a secondary star is one paradigm to explain a sub-class of jets in Planetary Nebulae and X-ray binaries. We consider an AGB primary and a main sequence secondary star with separations of order 20AU. As the stars orbit, the primary ejects a dense spherical wind and some of this material is captured by the secondary forming an accretion disk. The AMR allows us to follow the disk flow down to scales of order 0.2 AU. We investigate the distribution of the disks' density and velocity fields, as well as their accretion rates and angular momenta as a function of orbital period. Our calculations seem to suggest that the disk's total angular momentum vector tilts as the simulations evolve.

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