V3885 Sagittarius: a Comparison with a Range of Standard Model Accretion Disks

Abstract

A ${\tilde{\chi }}^2$ analysis of standard model accretion disk synthetic spectrum fits to combined $FUSE$ and STIS spectra of V3885 Sagittarius, on an absolute flux basis, selects a model that accurately represents the observed SED. Calculation of the synthetic spectrum requires the following system parameters. The cataclysmic variable secondary star period-mass relation calibrated by Knigge in 2007 sets the secondary component mass. A mean white dwarf (WD) mass from the same study, that is consistent with an observationally-determined mass ratio, sets the adopted WD mass of $0.7M_{\odot }$, and the WD radius follows from standard theoretical models. The adopted inclination, $i=65{\arcdeg}$, is a literature consensus, and is subsequently supported by ${\tilde{\chi }}^2$ analysis. The mass transfer rate is the remaining parameter to set the accretion disk $T_{\mathrm{eff}}$ profile, and the $Hipparcos$ parallax constrains that parameter to $\dot{M}=5.0\pm 2.0\times 10^{-9}{M}_{\odot }{\mathrm{yr}}^{-1}$ by a comparison with observed spectra. The fit to the observed spectra adopts the contribution of a $57,000\pm 5000$K WD. The model thus provides realistic constraints on $\dot{M}$ and $T_{\mathrm{eff}}$ for a large $\dot{M}$ system above the period gap.

41 pages, 7 figures, 9 tables. Astrophysical Journal (accepted)

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