Dynamic processes in Be star atmospheres. I - 'Dimple' formation in the He I lambda 6678 line of lambda Eridani

Details Dynamic processes in Be star atmospheres. I - 'Dimple' formation in the He I lambda 6678 line of lambda Eridani Dynamic processes in Be star atmospheres. I - 'Dimple' formation in the He I lambda 6678 line of lambda Eridani

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...408..323s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 408, no. 1, p. 323-336.

Astronomy and Astrophysics

Astronomy

26

B Stars, Stellar Atmospheres, Stellar Physics, Stellar Spectra, Ultraviolet Astronomy, Ultraviolet Spectra, Helium, Line Spectra, Stellar Mass Ejection, Stellar Spectrophotometry

Scientific paper

Several examples of weakenings of the C IV and N V resonance lines are found to coincide with the appearance of lambda 6678 dimples. The absence of variations in other UV lines and in the UV continuum at the same time or nearly the same time argues against dimples being caused by thermal variations from the underlying star. It is instead suggested that the resonance line weakenings are caused by non-LTE effects associated with the condensation of high density structures at some elevation over the star. A simple model of an opaque, essentially stationary slab which backscatters lambda 6678 line radiation into a surrounding 'penumbral' region is presented. Lambda 6678 photons are scattered a second time in this region back into the observer's line of sight and in the process acquire the local projected Doppler shift from rotation. Slabs would probably produce too little emission to be easily detected in the H alpha profile. Their detection in strong He I lines seems the best strategy among early Be stars.

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