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Simultaneous Spectroscopy and Polarimetry of Be Stars

  • D. R. Gies (a1) and David McDavid (a2)

Extract

Evidence is now accumulating that many Be stars display photospheric line profile variations on timescales of days or less that are probably caused by nonradial pulsations (Baade 1984; Penrod 1986). In some circumstances these pulsations can promote mass loss into the circumstellar envelope, and consequently the conditions in the inner part of the envelope may vary on similar timescales. Changes in the envelope could produce variations in the polarization and emission line profiles, and observers have reported rapid variability in both. We describe here an initial attempt to search for simultaneous variations in continuum polarization, Hα emission, and the He I λ6678 photospheric absorption line in order to investigate correlated changes on short timescales.

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References

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Baade, D. (1984). There are more absorption line profile-variable Be stars with short periods. Astr. Astrophys., 134, 105-17.
Hayes, D. P. and Guinan, E. F. (1984). The morphology of a mass loss episode of the Be star ω Ori. Astrophys. J., 279, 721-8.
McLean, I. S. (1979). Interpretation of the intrinsic polarizations of early-type emission-line stars. Mon. Not. R. Astr. Soc., 186, 265-85.
Penrod, G. D. (1986). Episodic mass motions and surface phenomenon. Pub. Astr. Soc. Pac., 98, 35-6.
Poeckert, R. (1981). A spectroscopic study of the binary Be star ϕ Persei. Pub. Astr. Soc. Pac., 93, 297317.
Poeckert, R., Bastien, P. and Landstreet, J. D. (1979). Intrinsic polarization of Be stars. Astr. J., 84, 812-30.

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