Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990acaps..10..154h&link_type=abstract
Acta Astrophys. Sin., Vol. 10, No. 2, p. 154 - 162
Astronomy and Astrophysics
Astrophysics
5
Be Stars: Infrared Excesses, Be Stars: Classification
Scientific paper
The infrared excess is one of the important characters of Be stars. The free-free radiation due to the interaction between the high temperature stellar wind and the low temperature gas disc is used to explain the infrared excess of Be stars. Be stars on the infrared color-color diagram should be distributed in a small special area. All Be stars listed in Jaschek and Egret (1982) and those with available IRAS flux densities at 12, 25, and 60 μm are plotted. It is easy to distinguish all 64 Be stars in two groups: the first group consists of Be stars, whose infrared excess can be explained as the radiation from free-free transition of gas disc. The Be stars of the second group are located outside the special area in the infrared color-color diagram. This result means that their infrared excess is not only due to the free-free radiation. The reasonable explanation is the thermal reradiation of circumstellar dust grains caused by absorption of UV and visual photons from the central stars.
Hu Jing-Yao
Xu Zhou
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