Accretion wake of 31 Cygni

Journal Article · Wed Mar 01 04:00:00 EST 1989 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/167253· OSTI ID:6018983

Ahmad, I A

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. 17 references.

• Research Organization: Imad-ad-Dean, Inc., Bethesda, MD (USA)
• OSTI ID: 6018983
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 338; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ABSORPTION SPECTRA
BINARY STARS
COSMIC RAY SOURCES
COSMIC X-RAY SOURCES
GIANT STARS
SHOCK WAVES
SPECTRA
STAR ACCRETION
STAR EVOLUTION
STARS
STELLAR ACTIVITY
STELLAR WINDS
SUPERGIANT STARS
ULTRAVIOLET SPECTRA