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RW Aur A, a close binary?

Title
RW Aur A, a close binary?
Type
Another Publication in an International Scientific Journal
Year
1999
Authors
Gahm, GF
(Author)
Other
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Petrov, PP
(Author)
Other
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Duemmler, R
(Author)
Other
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Gameiro, JF
(Author)
FCUP
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Journal
Vol. 352
Pages: L95-L98
ISSN: 0004-6361
Publisher: EDP Sciences
Scientific classification
FOS: Natural sciences > Physical sciences
Other information
Authenticus ID: P-001-2KE
Abstract (EN): We have discovered periodic changes in velocity and equivalent width of a number of different spectral features of RW Aur A, a T Tauri star with a jet, broad emission lines and substantial excess continuous emission. In particular, the photospheric lines vary in radial velocity with an amplitude of 5.7 km s(-1) over a period of 2.77 days, which appears to have been stable over at least 18 years. The present Letter focusses solely on one straightforward interpretation, namely that RW Am A is a single-lined spectroscopic binary. However, other spectral features vary in or out of phase with the same or the double period. Interpretations, other than a binary model, should be considered but must await the more extended report on our large observational material. In the binary case, the small amplitude leads to a mass function of only 5.10(-5) M., by far the smallest observed for young binaries. The jet velocity and extent restrict the range of inclinations (if the orbital axis is aligned with the jet), implying a close binary with a secondary at the brown dwarf limit. Further restrictions follow if the primary rotates synchronously. Narrow emission components of HeI and HeII vary in antiphase with the photospheric absorption lines. We show that it is unlikely that these lines reflect the motion of the secondary.
Language: English
Type (Professor's evaluation): Scientific
No. of pages: 4
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