The Episodic Dust-Maker WR:125 - Part Two - Spectroscopy and Photometry during Infrared Maximum

Bibcode
1994MNRAS.266..247W
Bouchet, P.; Kidger, M. R.; Geballe, T. R.; Williams, P. M.; van der Hucht, K. A.
Bibliographical reference

Monthly Notices of the Royal Astronomical Society, Vol. 266, NO. 1/JAN, P. 247, 1994

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1
1994
Journal
Monthly Notices of the Royal Astronomical Society
Number of authors
5
IAC number of authors
1
Citations
37
Refereed citations
30
Description
During 1992-93 the infrared flux from the Wolf-Rayet star WR 125, which formed a dust shell in 1990-91, reached a maximum. This is attributed to the continuous formation of dust in its wind until early 1993. Spectroscopy of the dust cloud in the 10-μm region showed that the expected WR emission lines were completely veiled by featureless emission from the heated dust. There was no evidence for silicate, silicon carbide or the narrow 11.52-μm graphite feature, supporting the view that the dust is amorphous carbon. An optical spectrum in the violet shows O II, He II and H absorption lines, confirming the deduction from the observed dilution of the WR emission lines that WR 125 is a binary system, and indicating a type of O9III for the companion to the WC7 star.
Type
Refereed

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