![Figure 10](f4_nomoto.png)
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.
![˙ M](article831x.gif)
![˙ ˙ ˙ Mstable ≲ M ≲ MRG](article832x.gif)
![M˙ ≲ M˙stable](article833x.gif)
![M˙](article834x.gif)
![M˙ ≳ M˙RG](article835x.gif)
![M˙ Edd](article836x.gif)
![MWD](article837x.gif)