Accretion in the zeta Aurigae and 32 Cygni shock cones

Details Accretion in the zeta Aurigae and 32 Cygni shock cones Accretion in the zeta Aurigae and 32 Cygni shock cones

Dec 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984nascp2349..357a&link_type=abstract

In its Future of Ultraviolet Astronomy Based on Six Years of IUE Res. p 357-360 (SEE N85-20961 11-89)

Astronomy and Astrophysics

Astronomy

Astronomical Models, Cygnus Constellation, Eclipsing Binary Stars, Stellar Mass Accretion, Zeta Aurigae Star, Angular Resolution, Dwarf Stars, Hot Stars, Magnesium, Supergiant Stars

Scientific paper

Zeta Aurigae and 32 Cygni are binary stars consisting of a cool supergiant primary and a hot dwarf secondary. Variations in the Mg II 2800 A and C IV 1550 A doublets of these stars near the time and secondary minimum were observed. Longward-shifted absorption is seen in the Mg II lines of both stars which may be due to material accreting onto the B star behind the shock front. A reverse P-Cygni profile in the C IV lines at some phases of zeta Aur was observed. This phenomenon seems transient and recurrent, and may suggest streaming. An abrupt strengthening and broadening of the absorption-especially at higher positive radial velocities-manifested in the CIV lines coincides with the onset and termination of the Mg II accretion absorption. It is suggested that this is the effect of the abrupt increase in optical depth as the line of sight aligns with the shock front. For 32 Cygni the observed aberration angle is similar to that of zeta Aur, but the system seems more diffucult to model. For zeta Aur the angle of aberration of the accreting material from the radial direction is about 38 deg. and the half width of the shock cone is about 11 deg. For 32 Cygni the aberration angle is about 44 deg.

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