Hot boundary layers in symbiotic binaries ax persei and ci cygni.

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 10 K, assuming for the accreting star a mass M* = 0.5 M0 and a radius R * = 0.2 R0. 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 (M = 1-10 x 10 M0 yr 1) but then stays nearly constant as the mass accretion rate approaches the Eddington limit (in the present case, MEdd 10- M0 yr `). 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 32 its expected value; the rest of the energy is advected into the star. Subject headings: accretion, accretion disks binaries: symbiotic stars: individual (AX Persei, CI Cygni)

Main Author: Godon, Patrick.
Format: Villanova Faculty Authorship
Language: English
Published: 1995
Online Access: http://ezproxy.villanova.edu/login?url=https://digital.library.villanova.edu/Item/vudl:176435
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dc_source_str_mv The Astrophysical Journal 462, May 1, 1996, 462-461.
author Godon, Patrick.
author_facet_str_mv Godon, Patrick.
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author_s Godon, Patrick.
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Hot boundary layers in symbiotic binaries ax persei and ci cygni.
author-letter Godon, Patrick.
author_sort_str Godon, Patrick.
dc_title_str Hot boundary layers in symbiotic binaries ax persei and ci cygni.
title Hot boundary layers in symbiotic binaries ax persei and ci cygni.
title_short Hot boundary layers in symbiotic binaries ax persei and ci cygni.
title_full Hot boundary layers in symbiotic binaries ax persei and ci cygni.
title_fullStr Hot boundary layers in symbiotic binaries ax persei and ci cygni.
title_full_unstemmed Hot boundary layers in symbiotic binaries ax persei and ci cygni.
collection_title_sort_str hot boundary layers in symbiotic binaries ax persei and ci cygni.
title_sort hot boundary layers in symbiotic binaries ax persei and ci cygni.
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description 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 10 K, assuming for the accreting star a mass M* = 0.5 M0 and a radius R * = 0.2 R0. 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 (M = 1-10 x 10 M0 yr 1) but then stays nearly constant as the mass accretion rate approaches the Eddington limit (in the present case, MEdd 10- M0 yr `). 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 32 its expected value; the rest of the energy is advected into the star. Subject headings: accretion, accretion disks binaries: symbiotic stars: individual (AX Persei, CI Cygni)
publishDate 1995
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dc.title Hot boundary layers in symbiotic binaries ax persei and ci cygni.
dc.creator Godon, Patrick.
dc.description 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 10 K, assuming for the accreting star a mass M* = 0.5 M0 and a radius R * = 0.2 R0. 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 (M = 1-10 x 10 M0 yr 1) but then stays nearly constant as the mass accretion rate approaches the Eddington limit (in the present case, MEdd 10- M0 yr `). 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 32 its expected value; the rest of the energy is advected into the star. Subject headings: accretion, accretion disks binaries: symbiotic stars: individual (AX Persei, CI Cygni)
dc.date 1995
dc.format Villanova Faculty Authorship
dc.identifier vudl:176435
dc.source The Astrophysical Journal 462, May 1, 1996, 462-461.
dc.language en
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