Figure 10: Limits of different burning regimes of accreted hydrogen onto a CO WD as a function
of mass of the WD and accretion rate 
[535]. If 
, hydrogen burns steadily.
If 
, H-burning shells are thermally unstable; with decrease of 
the strength of
flashes increases. For 
, hydrogen burns steadily but the excess of unburnt matter forms
an extended red-giant–sized envelope. In the latter case white dwarfs may lose matter by wind or
due to Roche lobe overflow. A dotted line shows the Eddington accretion rate 
as a function
of 
. The dashed lines are the loci of the hydrogen envelope mass at hydrogen ignition. Image
reproduced with permission from [535], copyright by AAS.
[535]. If , hydrogen burns steadily.
If , H-burning shells are thermally unstable; with decrease of the strength of
flashes increases. For , hydrogen burns steadily but the excess of unburnt matter forms
an extended red-giant–sized envelope. In the latter case white dwarfs may lose matter by wind or
due to Roche lobe overflow. A dotted line shows the Eddington accretion rate as a function
of . The dashed lines are the loci of the hydrogen envelope mass at hydrogen ignition. Image
reproduced with permission from [535], copyright by AAS.Konstantin A. Postnov and Lev R. Yungelson, "The Evolution of Compact Binary Star Systems",
Living Rev. Relativity, 17 (2014), 3, doi:10.12942/lrr-2014-3, URL (accessed <date>): http://www.livingreviews.org/lrr-2014-3.
This work is licensed under a Creative Commons License.
© The author(s), except where otherwise noted.
Living Rev. Relativity, 17 (2014), 3, doi:10.12942/lrr-2014-3, URL (accessed <date>): http://www.livingreviews.org/lrr-2014-3.
This work is licensed under a Creative Commons License.
© The author(s), except where otherwise noted.