Mass loss and mass transfer in the binary star HD 41335

Astronomy and Astrophysics – Astronomy

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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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