Other
Scientific paper
Jan 2012
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21915322m&link_type=abstract
American Astronomical Society, AAS Meeting #219, #153.22
Other
Scientific paper
In order to determine the amount of mass lost from a star which just fills its Roche Lobe, it is imperative to accurately calculate the size of the nozzle -- the area through which the mass flows. This is normally bounded by the equipotential surface where the density of the exponential atmosphere drops by one scale height. When the stars are in an eccentric orbit, Sepinsky et al. (2007) found that the equipotential surfaces defining the peanut-shaped shell ordinarily enclosing the two stars can "open up", no longer enclosing both stars. Furthermore, when attempting to calculate the orbit-variable mass transfer rate for eccentric systems, Haggerty and Sepinsky (2011) discovered that the equipotential surface defining the outer edge of the nozzle may "open up” -- and that this can occur closer to the donor star than its inner Lagrangian point (L1). In such a case, the nozzle is undefined at L1. Here, we develop a method for calculating the effective area of mass transfer by finding the area of the rings bounded at small radii by the Roche Lobe of the donor and at large radii by the equipotential surface. We calculate the area of the ring and its proximity to the L1 point as a function of eccentricity and the binary parameters. We then compare the mass transfer rate calculated for this area to other recent calculations of the mass transfer rate in eccentric binaries.
Haggerty Colby
Mancini Alyssa
Sepinsky J.
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