Hot Boundary Layers in Symbiotic Binaries AX Persei and CI Cygni

Details Hot Boundary Layers in Symbiotic Binaries AX Persei and CI Cygni Hot Boundary Layers in Symbiotic Binaries AX Persei and CI Cygni

May 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...462..456g&link_type=abstract

Astrophysical Journal v.462, p.456

Astronomy and Astrophysics

Astronomy

8

Accretion, Accretion Disks, Stars: Binaries: Symbiotic, Stars: Individual Constellation Name: Ax Persei, Stars: Individual Constellation Name: Ci Cygni

Scientific paper

Accretion disk boundary layer models are calculated for the symbiotic binaries AX Per and CI Cyg, using a time-dependent numerical code. Hot boundary layers are found with temperatures above 105 K, assuming for the accreting star a mass M* = 0.5 Msun and a radius R* = 0.2 Rsun. However, choosing a larger stellar radius or a smaller stellar mass leads to cooler boundary layers. The numerical solutions agree fairly well with the observational estimates of the hot component temperature during quiescence but do not reproduce the apparent drop in effective temperature seen during the outburst of AX Per and CI Cyg. The maximum effective temperature obtained in the boundary layer solutions increases as the mass accretion rate increases (Mdot = 1-10 x 10-5 Msun yr-1) but then stays nearly constant as the mass accretion rate approaches the Eddington limit (in the present case, MdotEdd ≍ 10-4 Msun yr-1). In this high accretion rate regime, the disk becomes geometrically thick (H/r ≍ 0.4), and the energy dissipated in the dynamical boundary layer is radiated outward to larger radii and advected into the star. The boundary layer luminosity is only ≍ ⅔ its expected value; the rest of the energy is advected into the star.

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