The optical counterpart of 3A0726-260 (4U0728-25)

Details The optical counterpart of 3A0726-260 (4U0728-25) The optical counterpart of 3A0726-260 (4U0728-25)

Feb 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...131..385c&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 131, no. 2, Feb. 1984, p. 385-389. Research supported by the Science and Engin

Astronomy and Astrophysics

Astrophysics

9

B Stars, Binary Stars, Stellar Spectra, X Ray Sources, Astronomical Photometry, Distance, Emission Spectra, H Lines, Interstellar Extinction, Neutron Stars

Scientific paper

The star 3A0726-260 is a member of the class of Be stars having strong X-ray emission. It is thought that the X radiation in this type of system is produced by accretion of matter from the envelope of the Be star onto a neutron star binary companion. It could thus be expected that the X-ray emission of 3A0726-260 would be pulsed with the rotation period of the neutron star, in common with other members of the class. The orbit in a number of these systems is found to be eccentric, and the amount of X-ray emission increases near periastron. For this type of binary system, the orbital period is generally tens to hundreds of days. While Steiner et al. (1983) observed H-beta to be in absorption in 3A0726-260, weak emission is observed.

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