Journal Article

On the nature of the Be star HR 7409 (7 Vul)

S. Vennes, A. Kawka, S. Jonić, I. Pirković, L. Iliev, J. Kubát, M. Šlechta, P. Németh and M. Kraus

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 413, issue 4, pages 2760-2766
Published in print June 2011 | ISSN: 0035-8711
Published online May 2011 | e-ISSN: 1365-2966 | DOI:
On the nature of the Be star HR 7409 (7 Vul)

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HR 7409 (7 Vul) is a newly identified Be star, possibly part of the Gould Belt, and is the massive component of a 69-d spectroscopic binary. The binary parameters and properties of the Be star measured using high-dispersion spectra obtained at Ondřejov Observatory and at Rozhen Observatory imply the presence of a low-mass companion (≈0.5–0.8 M). If the pair is relatively young (<50–80 Myr), then the companion is a K V star, but, following another, older evolutionary scenario, the companion is a horizontal branch star or possibly a white dwarf star. In the latter scenario, a past episode of mass transfer from an evolved star on to a less massive dwarf star would be responsible for the peculiar nature of the present-day, fast-rotating Be star.

Keywords: stars: emission-line, Be; stars: individual: HR 7409

Journal Article.  4604 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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