Issue |
A&A
Volume 367, Number 2, February IV 2001
|
|
---|---|---|
Page(s) | 549 - 556 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20000464 | |
Published online | 15 February 2001 |
On the origin of quiescent X-ray emission from A0535+26
1
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
2
Central Astronomical Observatory of the Russian Academy of Science at Pulkovo, Pulkovo 65-1, 196140 Saint-Petersburg, Russia
Corresponding author: N. R. Ikhsanov, ikhsanov@mpifr-bonn.mpg.de
Received:
9
October
2000
Accepted:
5
December
2000
The quiescent X-ray emission from A0535+26
() is explored in terms of
the spherically symmetrical accretion onto a magnetized neutron
star. I find the magnetospheric boundary of the neutron star in
A0535+26 to be stable with respect to interchange instabilities.
The fastest mode by which the accreting plas ma can enter the
magnetosphere is the magnetic lines reconnection. Under this
condition the quiescent X-ray luminosity of the system can be
explained provided the mass capture rate by the neutron star
from the wind of the Be companion of
∼
. I show this value to be in
a good agreement with the mass capture rate independently
evaluated from the established parameters of the Be star
circumstellar environment. The suggested approach allows to interpret
the low luminous state of the system
(
) in August -November 1998
in terms of the accretion powered pulsar model. I find the mass
capture rate by the neutron star during this time of
. This can be realized provided the
plasma density in the circumstellar disk of the Be companion is by
two orders of magnitude smaller than its average value. Under this
condition the disk is expected to be invisible in the optical/IR.
Key words: accretion / magnetic fields / stars: close binaries / stars: Be / stars: neutron star
© ESO, 2001
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