The accretion wake of 31 Cygni

Details The accretion wake of 31 Cygni The accretion wake of 31 Cygni

Mar 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...338.1011a&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 338, March 15, 1989, p. 1011-1015.

Astronomy and Astrophysics

Astrophysics

7

Cygnus Constellation, Eclipsing Binary Stars, Iue, Stellar Mass Accretion, Ultraviolet Spectra, Stellar Winds, Supergiant Stars, X Ray Binaries

Scientific paper

Archival IUE observations of 31 Cygni at phases at which its sister Zeta Aurigae systems exhibit evidence of an accretion wake are discussed. The absence of absorption in Mg II can be explained by the phase at the specific times of observation. The detection of high-velocity absorption due to C IV but not N V implies a shock temperature lower than that of Zeta Aur and 22 Vul but higher than than of 32 Cygni. The dependence of the high-velocity absorption component on phase is consistent with a simple model for the shock structure. The reverse P Cygni profiles in the high-temperature lines are weak and the emission components are observed only at the times when the accretion shock cone absorption is detected. Interpretation of a high-velocity shortward-shifted absorption component as circumstellar material is consistent with the estimated terminal velocity of the supergiant wind.

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