On the mass transfer  orbital period relation in cataclysmic variables.
Abstract
A simple method to obtain mass transfer rates in cataclysmic variables is discussed. The temperature T(R) of a steady accretion disc varies as R^{3/4}, leading to a connection between the accretion rate, the external radius R_{e} and the mean temperature of the disc, M ∝ R_{e}^{3} T_{m}^{4}. We find that if the disc size is a roughly constant fraction of the binary separation then R_{e} ∝ P^{2/3} and < ∝ T_{m}^{4} P^{2}. We argue from theoretical and observational reasons that there is no correlation between T_{m} and P, leading to the conclusion that M ∝ P_{2}. Since the radius of the secondary star is a function of the orbital period, we find that the mass transfer is directly proportional to the surface area of the companion star: M ∝ A_{8}. We use emission lines and photometry to estimate T_{m} and to calculate mass transfer rates for a large sample of cataclysmic variables, and compare the results with other authors.
 Publication:

Revista Mexicana de Astronomia y Astrofisica
 Pub Date:
 October 1994
 Bibcode:
 1994RMxAA..28..125E
 Keywords:

 Cataclysmic Binaries: Mass Transfer;
 Cataclysmic Binaries: Orbital Periods;
 Cataclysmic Binaries: Accretion Disks;
 Cataclysmic Binaries: Eclipsing Binaries;
 ACCRETION;
 ACCRETION DISKS;
 NOVAE;
 CATACLYSMIC VARIABLES