Volume 566, June 2014
|Number of page(s)||7|
|Published online||12 June 2014|
Relativistic effects on radiative ejection of coronae in variable X-ray sources
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warszawa, Poland
e-mail: email@example.com; firstname.lastname@example.org
Received: 1 July 2013
Accepted: 13 March 2014
Context. Optically thin coronae around neutron stars suffering an X-ray burst can be ejected as a result of rapid increase in stellar luminosity. In general relativity, radiation pressure from the central luminous star counteracts gravitational attraction more strongly than in Newtonian physics. However, motion near the neutron star is very effectively impeded by the radiation field.
Aims. To explore the mechanisms leading to ejection of accretion disk coronae
Methods. We perform a general relativistic calculation of the motion of a test particle in a spherically symmetric radiation field.
Results. At every radial distance from the star larger than that of the innermost stable circular orbit (ISCO), and any initial luminosity of the star, there exists a luminosity change which leads to coronal ejection. The luminosity required to eject from the system the inner parts of the optically thin neutron-star corona is very high in the presence of radiation drag and always close to the Eddington luminosity. Outer parts of the corona, at a distance of 20 RG or more, will be ejected by a sub-Eddington outburst. Mildly fluctuating luminosity will lead to dissipation in the plasma and may explain the observed X-ray temperatures of coronae in low mass X-ray binaries. At large radial distances from the star (3 × 103 RG or more) the results do not depend on whether or not Poynting-Robertson drag is included in the calculation.
Key words: stars: neutron / stars: winds, outflows / X-rays: binaries / X-rays: bursts / scattering / accretion, accretion disks
© ESO, 2014
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