Dwarf Novae with Newly Determined Parallaxes: Model Analyses of VY Aquarii, RU Pegasi, and T Leonis

Using newly determined parallaxes for dwarf novae, we have derived outburst accretion rates for VY Aqr, RU Peg, and T Leo, and for T Leo during quiescence. The two short‐period dwarf novae, VY Aqr and T Leo, show good agreement with optically thick steady‐state accretion disks in outburst, whereas RU Peg shows a significant departure from a steady‐state disk. We have determined that the white dwarf in T Leo has \documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackage[OT2,OT1]{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{empty} \DeclareMathSizes{10}{9}{7}{6} \begin{document} \landscape $T_{\mathrm{eff}\,}=16,000\pm 1000$ \end{document} K, a value consistent with long‐term compressional heating when gravitational‐wave emission drives mass transfer. The white dwarf in T Leo has a temperature in the same narrow range as other WZ Sge–like dwarf novae.