The recurrent nova U Scorpii post-outburst quiescence

Details The recurrent nova U Scorpii post-outburst quiescence The recurrent nova U Scorpii post-outburst quiescence

Mar 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985mnras.213..443h&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 213, March 15, 1985, p. 443-449.

Physics

Optics

46

Infrared Astronomy, Novae, Stellar Color, Stellar Luminosity, Stellar Spectra, Stellar Spectrophotometry, Cassegrain Optics, Companion Stars, Dwarf Stars

Scientific paper

A low-dispersion spectrum is presented for the recurrent nova U Scorpii after its return to post-outburst quiescence. The measured brightness and observed spectral features are the same as when it was observed serendipitously before the 1979 outburst. The spectrum shows He II emission lines on a nearly featureless continuum; as reported earlier by Williams et al. (1981), hydrogen is seen neither in emission nor in absorption. A spectral type of G0 (±5) V is inferred from identified absorption features (Ca H and K lines, the Mg b triplet) and JHK infrared photometry; however, it is not possible to rule out a giant star as the companion object. If it is indeed a dwarf, U Sco lies at a distance of ≡3.5±1.5 kpc.

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