Modeling accretional heating in dwarf novae.

We present a grid of evolutionary models of white dwarfs in cataclysmic variables undergoing accretional heating due to periodic dwarf nova events. Our quasi-static evolutionary sequences incorporate time-variable accretion, compressional heating, and boundary layer irradiation, including the effect of the stellar rotational velocity. The thermal evolution of a white dwarf is followed over many dwarf nova accretion cycles. We assess the effect of accretional heating on the surface observables of the accreting white dwarf as a function of the accretor mass, initial surface temperature, and accretion rate. We compare our theoretical results with recent observations of two systems, both in decline from an outburst of 12 days duration: RX And and U Gem. In order for the theoretical results to fit the observations, we find that RX and must have a massive white dwarf accretor (_1.2M_). For U Gem the parameters of the white dwarf, particularly the white dwarf mass and temperature, are accurately known, and this leads to a mass accretion rate of 3:0 _ 10_10 M_ yr_1 during the decline phase, i.e., 20 times smaller than its outburst value.

Main Author: Godon, Patrick.
Other Authors: Sion, Edward.
Language: English
Published: 2002
Online Access: http://ezproxy.villanova.edu/login?url=https://digital.library.villanova.edu/Item/vudl:176447
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dc_source_str_mv The Astrophysical Journal 586, March 20, 2003 421-431.
author Godon, Patrick.
author_facet_str_mv Godon, Patrick.
Sion, Edward.
author_or_contributor_facet_str_mv Godon, Patrick.
Sion, Edward.
author_s Godon, Patrick.
spellingShingle Godon, Patrick.
Modeling accretional heating in dwarf novae.
author-letter Godon, Patrick.
author_sort_str Godon, Patrick.
author2 Sion, Edward.
author2Str Sion, Edward.
dc_title_str Modeling accretional heating in dwarf novae.
title Modeling accretional heating in dwarf novae.
title_short Modeling accretional heating in dwarf novae.
title_full Modeling accretional heating in dwarf novae.
title_fullStr Modeling accretional heating in dwarf novae.
title_full_unstemmed Modeling accretional heating in dwarf novae.
collection_title_sort_str modeling accretional heating in dwarf novae.
title_sort modeling accretional heating in dwarf novae.
description We present a grid of evolutionary models of white dwarfs in cataclysmic variables undergoing accretional heating due to periodic dwarf nova events. Our quasi-static evolutionary sequences incorporate time-variable accretion, compressional heating, and boundary layer irradiation, including the effect of the stellar rotational velocity. The thermal evolution of a white dwarf is followed over many dwarf nova accretion cycles. We assess the effect of accretional heating on the surface observables of the accreting white dwarf as a function of the accretor mass, initial surface temperature, and accretion rate. We compare our theoretical results with recent observations of two systems, both in decline from an outburst of 12 days duration: RX And and U Gem. In order for the theoretical results to fit the observations, we find that RX and must have a massive white dwarf accretor (_1.2M_). For U Gem the parameters of the white dwarf, particularly the white dwarf mass and temperature, are accurately known, and this leads to a mass accretion rate of 3:0 _ 10_10 M_ yr_1 during the decline phase, i.e., 20 times smaller than its outburst value.
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dc.title Modeling accretional heating in dwarf novae.
dc.creator Godon, Patrick.
Sion, Edward.
dc.description We present a grid of evolutionary models of white dwarfs in cataclysmic variables undergoing accretional heating due to periodic dwarf nova events. Our quasi-static evolutionary sequences incorporate time-variable accretion, compressional heating, and boundary layer irradiation, including the effect of the stellar rotational velocity. The thermal evolution of a white dwarf is followed over many dwarf nova accretion cycles. We assess the effect of accretional heating on the surface observables of the accreting white dwarf as a function of the accretor mass, initial surface temperature, and accretion rate. We compare our theoretical results with recent observations of two systems, both in decline from an outburst of 12 days duration: RX And and U Gem. In order for the theoretical results to fit the observations, we find that RX and must have a massive white dwarf accretor (_1.2M_). For U Gem the parameters of the white dwarf, particularly the white dwarf mass and temperature, are accurately known, and this leads to a mass accretion rate of 3:0 _ 10_10 M_ yr_1 during the decline phase, i.e., 20 times smaller than its outburst value.
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dc.source The Astrophysical Journal 586, March 20, 2003 421-431.
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