Mass loss and mass transfer in the binary star HD 41335

Details Mass loss and mass transfer in the binary star HD 41335 Mass loss and mass transfer in the binary star HD 41335

Apr 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980esasp.157...51p&link_type=abstract

The second European International Ultraviolet Explorer (IUE) Conference, held 26-28 March 1980 in Tübingen, West Germany. Edited

Astronomy and Astrophysics

Astronomy

3

Binary Stars, Iue, Mass Transfer, Stellar Mass Ejection, Ultraviolet Astronomy, Absorption Spectra, Aluminum, Carbon, Iron, Photosphere, Silicon, Stellar Envelopes, Stellar Winds

Scientific paper

The Be star HD 41335, a prototype of an interacting binary, is discussed. International Ultraviolet Explorer high resolution spectra obtained at 5 different phases of the binary cycle show prominent variations due to the transfer of mass between the secondary and the primary star (B2V). Redshifted (V = +50 km/s) narrow lines are characteristics of the phase 0 (primary seen through the mass flow). Around phase 0.5, blueshifted shell lines (V = -65 km/s) indicate a mass flow through the external Lagrangian point. The Al 3 (1), Si 4 (1), C4 (1), Fe 3 (34, 38) multiplets present at all the phases strong and asymmetric absorption features, with outward velocities up to 550 km/s (C4), larger than the escape velocity for this rapidity rotating star (v sin i + 415 km/s).

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