Low-mass X-ray binary models for the supersoft X-ray sources CAL 83, CAL 87 and RX J0527.8-6954 in the Large Magellanic Cloud

Details Low-mass X-ray binary models for the supersoft X-ray sources CAL 83, CAL 87 and RX J0527.8-6954 in the Large Magellanic Cloud Low-mass X-ray binary models for the supersoft X-ray sources CAL 83, CAL 87 and RX J0527.8-6954 in the Large Magellanic Cloud

Nov 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...278l..43k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 278, no. 2, p. L43-L46

Astronomy and Astrophysics

Astronomy

35

Eddington Approximation, Magellanic Clouds, Neutron Stars, Stellar Mass Accretion, Stellar Models, X Ray Astronomy, X Ray Binaries, X Ray Spectra, Optical Thickness, Rosat Mission, Stellar Luminosity, Stellar Magnetic Fields

Scientific paper

We have performed detailed numerical calculations of sub-Eddington spherical accretion onto neutron stars and computed the emergent spectra. We have found that the supersoft X-ray spectra observed in CAL 83, CAL 87 and RX J0527.8-6954 can be explained as the result of near-Eddington accretion onto neutron stars. Our model is consistent with a recently proposed unified model for the Low-Mass X-ray Binaries (LMXRB). If the luminosity of the source is within 10% of the Eddington value, the crucial parameter that determines whether the source appears as a 'canonical' LMXRB or as a supersoft X-ray source is the extent of the matter that accretes radially. If the radial flow extends to at most a few hundred neutron star radii, the source exhibits the characteristics of a 'canonical' LMXRB. If on the other hand the radial flow extends to at least a few thousand neutron star radii the source behaves like a supersoft one. In this last case the effective optical depth to absorption is larger than one throughout the flow, the photosphere moves out to large radii and the emitted spectrum is a blackbody with temperature in the tens of eV range.

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