UV and X-ray emission in the interacting binary U Cephei

Details UV and X-ray emission in the interacting binary U Cephei UV and X-ray emission in the interacting binary U Cephei

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26as...97..261g&link_type=abstract

Astronomy and Astrophysics Supplement Series (ISSN 0365-0138), vol. 97, no. 1, p. 261-263.

Astronomy and Astrophysics

Astrophysics

Eclipsing Binary Stars, Emission Spectra, Stellar Activity, Ultraviolet Emission, X Ray Spectra, High Temperature Plasmas, Late Stars, Spectral Line Width, Stellar Coronas, Stellar Spectra

Scientific paper

The active close binary U Cep has been monitored in the ultraviolet, using IUE, during 1.25 orbital cycles. The emission spectrum at the bottom of the primary total eclipse confirms earlier suggestions of an unexpected absence of the Hell 1640 A line. Stronger than expected emission in some other lines like NV, CII, CIV or AlIII, indicative of hot plasma, points out that some important differences still remain between the active components of RS CVn-type binaries and the mass-losing components of semidetached Algols. Simultaneous X-ray measurements, carried out with GINGA, indicated a low upper limit flux in the observed energy range (1 to 10 keV). A comparison with other binary systems or isolated stars is discussed in order to understand the obtained results.

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