Issue |
A&A
Volume 375, Number 2, August IV 2001
|
|
---|---|---|
Page(s) | 419 - 433 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20010838 | |
Published online | 15 August 2001 |
The soft X-ray eclipses of HU Aqr
1
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
2
Space Sciences Laboratory, UC Berkeley, CA 94720, USA
3
Planetary Science Institute, Tucson, AZ 85705, USA
Corresponding author: A. D. Schwope, aschwope@aip.de
Received:
21
March
2001
Accepted:
7
June
2001
We present the results of extended monitoring observations
in soft X-rays of the bright eclipsing polar (AM Herculis star)
HU Aqr. It was observed between 1990 and 1998
by ROSAT for a total of 230 ksec using the PSPC
and the HRI detectors and by EUVE with the Deep Survey Imager and the
Spectrometer for a total of 580 ksec.
The overall X-ray brightness of HU Aqr varied due to changes of the
mass accretion rate by a factor of 40 over that period of time.
At all occasions the X-ray light curve was characterized by a marked
on-off behavior due to the self-eclipse of the accreting pole.
The X-ray light curve showed eclipses by the companion star, the
accretion stream and by an accretion curtain raised between the
two stars in the binary.
Narrow dips prior to the stellar eclipse
are caused by the transit of the outer accretion stream. These
dips display marked phase shifts,
thus indicating a large movement of the threading region, where the
stream couples to the magnetic field. These shifts are shown
to be related to changes of the mass accretion rate.
Correspondingly,
the spot longitude varied between 34°and 50°.
The X-ray light curves display clear evidence for the presence of an accretion
curtain, which is raised all along the ballistic accretion stream down to the
region where the bulk of matter couples onto magnetic field lines.
A lower limit to the mass accretion rate in the curtain is
/yr, which is of order 10% of the total mass
accretion rate.
A linear fit to all available eclipse egress times yields an updated
orbital ephemeris of the system:
with T0 the time of eclipse of the white dwarf centre of mass
(BJED: barycentric Julian ephemeris time).
The inclusion of a quadratic term gives a better fit to the data but
is not regarded as indication of a period change or asynchronous rotation
but by a migration of the
accretion spot over the surface of the white dwarf.
For one particular data set obtained in a high accretion state, detailed
light curve modeling was possible.
The egress from eclipse lasted 1.3 s,
which constrained the azimuthal extent of the accretion spot to less than
4°or 450 km. The spot extended vertically by ≤0.015 Rwd. A comparison of the width of the stream dip and the extent of the accretion spot
shows, that only the inner 60-80% of the stream are dense enough
to fire the soft X-ray engine.
During the eclipse, HU Aqr was detected at a flux level of
erg cm-1 s-1. The implied
X-ray luminosity is
erg s-1,
comparable with X-ray emission from single, late-type, active stars.
Key words: accretion, accretion disks / stars: binaries: eclipsing / stars: novae, cataclysmic variables / stars: individual: HU Aqr / X-rays: binaries
© ESO, 2001
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