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| Paper: |
How Strong is Mass Loss from B[e] Stars? |
| Volume: |
388, Mass Loss from Stars and the Evolution of Stellar Clusters |
| Page: |
205 |
| Authors: |
Miroshnichenko, A. |
| Abstract: |
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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