Mass loss rate from IUE observations of Zeta AUR systems

Details Mass loss rate from IUE observations of Zeta AUR systems Mass loss rate from IUE observations of Zeta AUR systems

Jun 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982esasp.176..355c&link_type=abstract

In ESA 3rd European IUE Conf. p 355-357 (SEE N83-11889 02-88)

Mathematics

1

Binary Stars, Cygnus Constellation, Stellar Mass Ejection, Zeta Aurigae Star, Approximation, Branching (Mathematics), Iron, Iue, Parameterization, Photons, Resonance Lines, Stellar Winds, Supergiant Stars, Wind Velocity

Scientific paper

A method which determines the mass loss rate of the red supergiant in Zeta Aur systems, using resonance lines, is presented. The method exploits a three dimensional nonspherical line transfer code. The wind is assumed to be expanding spherically. The line source function is treated by Sobolev approximation. The Fe II UV mult. 9 photon lines are used. Due to the unfavorable branching ratio these are emitted as mult. 191 lines. Observed equivalent widths of the absorption lines are matched with theoretical line strengths parametrized by mass loss rate and stellar wind velocity. For 32 Cyg, mass loss rate = 0.000000018 M/yr, wind velocity = 40 km/sec, microturbulence velocity = 25 km/sec. For Zeta Aur, the values are 0.00000004 M/yr, 35 km/sec, and 30 km/sec for 31 Cyg, 0.000000017 M/yr, 40 km/sec, and 25 km/sec.

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