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Dust formation of Be stars with large infrared excess

Published online by Cambridge University Press:  12 July 2011

Chien-De Lee  and
Wen-Ping Chen
Chien-De Lee
Affiliation:
Graduate Institute of Astronomy, National Central University, Jhongli 32001, Taiwan email: m959009@astro.ncu.edu.tw
Wen-Ping Chen
Affiliation:
Graduate Institute of Astronomy, National Central University, Jhongli 32001, Taiwan email: m959009@astro.ncu.edu.tw Department of Physics, National Central University, Jhongli 32001, Taiwan email: wchen@astro.nuc.edu.tw
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Abstract

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Classical Be stars, in addition to their emission-line spectra, are associated with infrared excess which is attributable to free-free emission from ionized gas. However, a few with exceptionally large near-infrared excess, namely with J–H, and H–Ks both greater than 0.6 mag—and excess emission extending to mid- and far-infrared wavelengths—must be accounted for by thermal emission from circumstellar dust. Evolved Be stars on the verge of turning off the main sequence may condense dust in their expanding cooling envelopes. The dust particles should be very small in size, hence reprocess starlight efficiently. This is in contrast to Herbig Ae/Be stars for which the copious infrared excess arises from relatively large grains as part of the surplus star-forming materials.

Keywords

stars: early-typestars: evolutionstars: emission-lineBestars: pre–main-sequenceinfrared: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 366 - 371
Copyright
Copyright © International Astronomical Union 2011

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