Issue |
A&A
Volume 392, Number 2, September III 2002
|
|
---|---|---|
Page(s) | 541 - 551 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20011651 | |
Published online | 30 August 2002 |
A multiwavelength timing analysis of the eclipsing polar DP Leo
1
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
2
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, Germany
3
Deptartment of Physics and Astronomy, University of Southampton, Hampshire, Southampton, SO17 1BJ, UK
Corresponding author: A. D. Schwope, aschwope@aip.de
Received:
3
August
2001
Accepted:
17
June
2002
We present an analysis of the X-ray light curves of the
magnetic cataclysmic variable DP Leo using recently
performed XMM-Newton EPIC and archival published and unpublished
ROSAT PSPC observations. We combine the timings of the X-ray eclipses
with timings derived from archival HST-observations and
new optical observations with the photon counting
OPTIMA camera.
We determine the eclipse length at X-ray wavelengths to be s,
slightly longer than at ultra-violet wavelengths, where it lasts 225 s.
A new orbital ephemeris is derived which
connects the more than 120 000 binary cycles covered since 1979. It has
a highly significant quadratic term, implying an orbital period change
of
s s-1, two orders of magnitude larger
than being compatible with braking by gravitational radiation only.
Over the last twenty years, the optical and X-ray bright phases
display a continuous shift
with respect to the eclipse center by ~
yr-1.
Over the last 8.5 years the shift of the X-ray bright phase
is ~
yr-1.
We interpret this as evidence of an asynchronously rotating
white dwarf although synchronization oscillations cannot
be ruled out completely. If the observed phase shift
continues, a fundamental rearrangement of the
accretion geometry must occur on a time-scale of some ten years.
Applying model atmosphere spectra to optical/UV eclipse light curves,
we determine the temperature and mass of the white dwarf,
the temperature and size of the optical/UV emitting
spot and the distance to DP Leo to be
K,
,
K,
, and
pc, respectively.
The implied inclination and mass ratio are
and
.
DP Leo is marginally detected at eclipse phase in X-rays.
The upper limit eclipse flux is consistent with an origin
on the late-type secondary,
(0.20-7.55 keV),
at a distance of 400 pc.
Key words: stars: binaries: eclipsing / stars: novae, cataclysmic variables / stars:individual: DP Leo / X-rays: stars
© ESO, 2002
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