Optical identification of the supersoft X-ray source RX J0439.8-6809.

Details Optical identification of the supersoft X-ray source RX J0439.8-6809. Optical identification of the supersoft X-ray source RX J0439.8-6809.

Mar 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...307l..49v&link_type=abstract

Astronomy and Astrophysics, v.307, p.L49-L52

Astronomy and Astrophysics

Astrophysics

9

Accretion, Stars: Individual: Rxj0439.8-6809, Stars: Post-Agb, White Dwarfs, X-Rays: Stars

Scientific paper

We have identified RXJ0439.X-6809 with a very blue B=21.5 object. There is no evidence for x-ray or optical variability. The optical spectrum does not show any absorption or emission features. The very blue optical spectrum suggests that the optical flux is the Rayleigh-Jeans tail of the soft X-ray component. The spectral parameters are consistent with a location in the Large Magellanic Cloud. RXJ0439 may be an accreting binary in which a low-mass white dwarf is recurrently burning accreted matter with a very long X-ray on-time. Alternatively, RXJ0439 may be a ~1Msun_ post-AGB star, which may have re-entered the high-luminosity phase due to a late helium shell flash.

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