How Strong is Mass Loss from B[e] Stars?

Details How Strong is Mass Loss from B[e] Stars? How Strong is Mass Loss from B[e] Stars?

Jun 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aspc..388..205m&link_type=abstract

Mass Loss from Stars and the Evolution of Stellar Clusters ASP Conference Series, Vol. 388, proceedings of the conference held 2

Astronomy and Astrophysics

Astronomy

2

Scientific paper

The B[e] phenomenon is defined as a combination of the presence of forbidden line emission and near-infrared excess in the spectra of B-type stars. It is observed in objects with extended gas-and-dust circumstellar envelopes at a wide range of evolutionary stages: from the pre-main-sequence to the post-AGB. The extremely strong Balmer emission lines in many, especially non-supergiant, B[e] stars may imply high mass loss rates, whose estimates are available for only a few such objects and do not agree with wind models and observational relationships published by Henny Lamers and collaborators. Here I review the existing mass loss rate determinations for B[e] stars and discuss ways to interpret the disagreement.

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