Optical/UV counterpart of the supersoft transient X-ray source RX J0513.9-6951 in the Large Magellanic Cloud

Details Optical/UV counterpart of the supersoft transient X-ray source RX J0513.9-6951 in the Large Magellanic Cloud Optical/UV counterpart of the supersoft transient X-ray source RX J0513.9-6951 in the Large Magellanic Cloud

Nov 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...278l..39p&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 278, no. 2, p. L39-L42

Astronomy and Astrophysics

Astronomy

54

Accretion Disks, B Stars, Blue Stars, Magellanic Clouds, Neutron Stars, Ultraviolet Photometry, Visible Spectrum, White Dwarf Stars, X Ray Sources, X Ray Spectra, Compton Effect, Iue, Line Spectra, Radial Velocity, Rosat Mission, Sky Surveys (Astronomy), Stellar Spectrophotometry, X Ray Telescopes

Scientific paper

Optical and IUE observations of the ROSAT X-ray transient RX J0513.9-6951 show this object to be remarkably similar to Cal 83, the prototype of luminous supersoft sources which is also located in the Large Magellanic Cloud (LMC). The counterpart is a B approx. = 17 mag blue star which apparently did not vary much around the time of the X-ray outburst. Spectrophotometry reveals narrow and broad emission lines of H, He II, N V, and O VI, whereas the lambda lambda 1548,50 C IV resonance doublet is very weak. Radial velocity variations by approx. = 100 km/s suggest binary nature and systemic velocity close to the bulk motion of the LMC. We discuss the hypothesis that the source is mainly powered by nuclear burning on the surface of a white dwarf rather than by accretion, and we argue that the X-ray outburst was triggered by a reduced accretion rate.

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