Accretion Flows and Disk Formation in Close Binary Systems

Details Accretion Flows and Disk Formation in Close Binary Systems Accretion Flows and Disk Formation in Close Binary Systems

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dps....41.4001d&link_type=abstract

American Astronomical Society, DPS meeting #41, #40.01

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Scientific paper

Binary systems are the typical outcome of star formation by fragmentation of dense cores in molecular clouds and accrete mass from the envelope via a circumbinary disk. We study the effects of accretion from a disk onto a close protobinary that has slightly different stellar masses. Line emission profiles from the circumstellar disk and accretion streams onto the components of a close T Tauri binary system are studied as a function of orbital phase. We use hydrodynamic two-dimensional simulations with an adaptive mesh refinement method to derive the density and velocity distributions of the circumbinary material. We assume that the gas is locally isothermal, with a temperature profile depending on the distance to the center of mass and to each stellar component. The shape of line profiles is estimated decoupled from the mass transfer dynamical simulations considering different contributions inside the circumbinary gap and assuming that line emissivity is proportional to the volume emission measure along the line of sight. Accretion across the low-density inner cavity occur in a time-dependent manner in our simulations. There is a fair agreement between our calculated profiles from the outer accretion regions and the observed time variability of optically thin Balmer line profiles in close binary systems. We conclude that substantial accretion can take place across the circumbinary gap in binary systems with a circular orbit, preferentially through the co-rotating Lagrangian points.

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