BALMER LINE EMISSION PROFILES FROM CATACLYSMIC VARIABLE ACCRETION DISK CHROMOSPHERES

Stark-broadened, emisson-line profiles are computed for physical condi tions extant in the chromospheres of cataclysmic variable accretion di sks. These calculations follow the methods of Lin, Williams, & Stover, except that our results span the lower electron number density range of 12 less than or equal to log n(e) (cm(-3)) less than or equal to 14 . The rationale for high Balmer line optical depths at accretion disk faces caused by photoionization from a source in the vicinity of the w hite dwarf is outlined; then a series of models based on accurate abso rption line coefficients is computed. Stark-broadened line widths of u p to several Doppler widths are found. These pressure-broadened profil es are enough to smear the classic double-cusped line profile signific antly for chromosphere temperatures of similar to 10,000 K, which are at the high end of those considered by Lin and coworkers. Emission-lin e profiles with greatly smoothed cusps result in all cases except in n early edge-on systems, where the mass accretion rate drops below 10(-1 0) M. yr(-1) or where the accretion disk outer radii are less than 10( 10.5) cm. These results are insensitive to the shape of the boundary l ayer energy distribution.