Ultraviolet and optical spectroscopy and polarimetry of the helium weak star HD 21669: Evidence for a magnetically controlled stellar wind

Details Ultraviolet and optical spectroscopy and polarimetry of the helium weak star HD 21669: Evidence for a magnetically controlled stellar wind Ultraviolet and optical spectroscopy and polarimetry of the helium weak star HD 21669: Evidence for a magnetically controlled stellar wind

Dec 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984nascp2349..483b&link_type=abstract

In NASA. Goddard Space Flight Center Future of Ultraviolet Astronomy Based on Six Years of IUE Res. p 483-486 (SEE N85-20961 1

Astronomy and Astrophysics

Astronomy

4

Polarimetry, Stellar Composition, Stellar Magnetic Fields, Stellar Winds, Ultraviolet Spectra, Visible Spectrum, Helium, Line Spectra, Magnetic Stars, Star Clusters, Stellar Mass, Stellar Rotation, Variations

Scientific paper

High dipsersion SWP spectra with IUE, and contemporaneous optical Zeeman polarimetry and spectroscopy of the helium weak star HD 21699 = HR 1063 were obtained. All IUE observations were made during Sept. 1983 and Feb. 1984. The C IV 1548,1550 doublet varies on a timescale consistent with the photometric and magnetic period, while no other strong lines in the UV display obvious variations in profile or strength. Only the helium weak star HD 5737 = alpha Scl shows a similarly strong C IV line among the helium weaks. This set of observations is discussed in the context of a magnetic star which is losing mass, having constrained that outflow to corotate with the stellar surface. If the magnetic period is correct, the greatest mass outflow seems to be from above the polar regions. The comparison between optical and UV spectrum phenomenology is also considered.

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