Correlation and variability of the He I 4471 and MG II 4481 absorption lines in Be stars - A possible diagnositc tool for nonradial pulsations

Details Correlation and variability of the He I 4471 and MG II 4481 absorption lines in Be stars - A possible diagnositc tool for nonradial pulsations Correlation and variability of the He I 4471 and MG II 4481 absorption lines in Be stars - A possible diagnositc tool for nonradial pulsations

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990ap%26ss.173..145v&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 173, no. 1, Nov. 1990, p. 145-156. Research supported by the Fondo Naciona

Astronomy and Astrophysics

Astrophysics

4

Absorption Spectra, B Stars, Helium, Magnesium, Stellar Oscillations, Spectral Line Width, Stellar Models, Stellar Rotation, Stellar Spectrophotometry

Scientific paper

In a total of 181 photographic spectrograms, obtained at the Manuel Foster Observatory of the Catholic University in Santiago (Chile), the equivalent widths of the absorption lines Hel 4471 and Mgii 4481 have been determined for 10 selected southern Be stars and 4 normal B-type stars. The mean equivalent widths of each star are compared to published mean values from larger samples of B stars. On the average, Be stars coincide with normal B-type stars in their equivalent width. However, a striking difference between rapidly and slowly rotating stars in their line ratios (HeI/MgII) was found, which is probably an artifact due to a systematic misclassification of spectral types of rapidly rotating B stars (v sini> 200 km s - 1). Six of the ten Be stars show evidence for variability in Hei and/or Mgii with time-scales shorter than a few days and amplitudes up to a factor 2 in equivalent width. Line variability occurs in the entire range of projected rotation velocity (70 km s - 1

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