| |
 |
| Paper: |
A Classical Nova Explosion in a Binary System with B[e] Star |
| Volume: |
447, Evolution of Compact Binaries |
| Page: |
227 |
| Authors: |
Filippova, E.; Revnivtsev, M.; Lutovinov, A. |
| Abstract: |
The description of a thermonuclear runaway on a white dwarf, which
causes a Classical Nova (CN) explosion, has several uncertainties.
Observational tests of models are
challenging because the majority of CNe are observed in optical
and NIR spectral bands days after the onset of the explosion. We propose to
use the properties of the X-ray emission of CNe for these tests.
We have developed a model for the 1998 CN explosion in the binary
system CI Cam. According to the adopted model the stellar wind from the
optical component (a B[e] star), heated by a strong shock wave that was
produced when matter was ejected from the white dwarf as the result of a
thermonuclear explosion on its surface, is the source of X-ray
emission in the standard X-ray band (∼ 2 - 10 keV).
We use this model to explain the behaviour of the X-ray luminosity and of
the mean temperature of the heated material during the explosion,
and obtain velocity and mass estimates of the ejected matter from the WD
surface. Discrepancies between model and observations, for example the
slower decline of the theoretical luminosity compared to the observed one,
are likely caused by the rough assumption of spherical symmetry. Using 3D
calculations we find possible density perturbations (accretion wakes) that
can reconcile theory with observations. |
|
|
|
|
|
