Abstract
We apply the Deloye & Bildsten isentropic models for donors in ultracompact low-mass X-ray binaries to the AM CVn population of ultracompact, interacting binaries. The mass-radius relations of these systems' donors in the mass range of interest (M<SUB>2</SUB><0.1M<SUB>solar</SUB>) are not single-valued, but parameterized by the donor's specific entropy. This produces a range in the relationships between system observables, such as orbital period P<SUB>orb</SUB> and mass transfer rate M˙. For a reasonable range in donor specific entropy, M˙ can range over several orders of magnitude at fixed P<SUB>orb</SUB>. We determine the unique relation between M˙ and M<SUB>2</SUB> in the AM CVn systems with known donor-to-accretor mass ratios q=M<SUB>2</SUB>/M<SUB>1</SUB>. We use structural arguments, as well as each system's photometric behavior, to place limits on M˙ and M<SUB>2</SUB> in each. Most systems allow a factor of about 3 variation in M˙, although V803 Cen, if the current estimates of its q are accurate, is an exception and must have M<SUB>2</SUB>~0.02M<SUB>solar</SUB> and M˙~10<SUP>-10</SUP>M<SUB>solar</SUB> yr<SUP>-1</SUP>. Our donor models also constrain each donor's core temperature (T<SUB>c</SUB>) range and correlate T<SUB>c</SUB> with M<SUB>2</SUB>. We examine how variations in donor specific entropy across the white dwarf family of AM CVn systems affects this population's current Galactic distribution. Allowing for donors that are not fully degenerate produces a shift in systems toward longer P<SUB>orb</SUB> and higher M˙, increasing the parameter space in which these systems can be found. This shift increases the fraction of systems whose P<SUB>orb</SUB> is long enough that their gravity wave (GW) signal is obscured by the background of detached double white dwarf binaries that dominate the GW spectrum below a frequency of ~2 mHz.
