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Paper: What Simulations Tell Us About White Dwarf Evolution in AM CVn Close Binaries
Volume: 509, 20th European Workshop on White Dwarfs (EuroWD16)
Page: 549
Authors: Montgomery, M. M.
Abstract: In this work, we review the three most likely evolutionary channels that may result in AM CVn close binaries leading to white dwarf supernovae as evolutionary endpoints. To determine the likely evolutionary path for an AM CVn system, masses are needed. To find the secondary-to-primary mass ratio, a recent hypothesis suggests using the positive superhump period from Stage A of the superoutburst light curve rather than Stage B. To determine the most likely evolutionary track for this system, we compare observational data with values from three 3D SPH numerical simulations, one simulation for each of the potential evolutionary channels for AM CVn system SDSS J090221.35+38941.9. In this work, we explain why the white dwarf channel may be eliminated for this system. As for the other two channels, we find that the simulated parameters for the CV channel looks most promising for the primary white dwarf J0902 to reach supernova type Ia. However, a comparison of simulated and observed positive superhump period excess values suggests that the helium star channel is more likely, although the results do not support a supernova as the white dwarf primary's endpoint.
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