Ultraviolet observations of the Be star MU Centauri during its recent active phase

Details Ultraviolet observations of the Be star MU Centauri during its recent active phase Ultraviolet observations of the Be star MU Centauri during its recent active phase

Dec 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984pasp...96..960p&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 96, Dec. 1984, p. 960-967.

Astronomy and Astrophysics

Astronomy

10

B Stars, Spaceborne Astronomy, Stellar Activity, Stellar Spectrophotometry, Ultraviolet Astronomy, Variable Stars, Balmer Series, Emission Spectra, H Alpha Line, Iue, Oao 3, Spectral Line Width, Spectrum Analysis, Stellar Envelopes

Scientific paper

IUE and Copernicus ultraviolet observations and ground-based image-tube and direct spectrograms of the pole-on Be star Mu Cen have been combined to investigate the nature of this star's activity during its Balmer emission-line episode of 1980-81. Within the uncertainties of the observations, the UV data show no evidence for a wind, a classical-type shell injection, or a region of superionization, either before, during, or after the active phase. This is contrary to current views on how the circumstellar envelopes in Be stars are produced. The only difference between the UV spectra observed during activity and quiescence was that the lines from the more highly ionized species (e.g., Si III, Si IV, Al III) were slightly stronger and broader when Balmer emission was present. Evidence is presented that the activity most likely resides in or near the photosphere, and that during such active periods the photospheric temperature is higher. The recently discovered nonradial pulsations in Mu Cen (Baade, 1984) may supply the energy. The lack of sharp or broad shell lines in the UV suggests that the Balmer emission envelope is at least somewhat flattened.

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