The peculiar O9.5V star BD+53°2790, the massive counterpart to the X-ray binary system 4U 2206+54

Details The peculiar O9.5V star BD+53°2790, the massive counterpart to the X-ray binary system 4U 2206+54 The peculiar O9.5V star BD+53°2790, the massive counterpart to the X-ray binary system 4U 2206+54

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011bsrsl..80..634b&link_type=abstract

Société Royale des Sciences de Liège, Bulletin, vol. 80, p. 634-638 (Proceedings of the 39th Liège Astrophysical Colloquium, hel

Astronomy and Astrophysics

Astrophysics

Scientific paper

The X-ray binary system 4U 2206+54 hides many mysteries. Among them, the surprising behavior of both of its co components: the O9.5 dwarf star BD+53°2790 and a slowly rotating neutron star. BD+53°2790 misled the astronomers, exhibiting characteristics reminiscent of Be stars. However, a deeper spectral analysis and more intense monitoring revealed that the real picture was a bit more complicated: a) Although it shows evidence of a circumstellar envelope, its observable properties differ from those typical of envelopes in Be stars. b) Comparison with spectral standards and models indicates a possible over-abundance in He. This would open the possibility to link the behavior of BD+53°2790 to the He-rich class of stars. c) UV spectra show an abnormally slow and dense wind for an O9.5V star. d) Spectral classification in the IR wavelength region suggest a more likely supergiant nature of the source, in contradiction with the optical classification. e) The presence of an intense magnetic field is under investigation. BD+53°2790 stands as a perfect laboratory for testing stellar structure, as well as wind and evolutionary theories. The observable properties of this source in a wide range of spectral bands are discussed, and some interpretations outlined.

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