This article has an erratum: [erratum]
Volume 368, Number 2, March III 2001
|Page(s)||471 - 483|
|Section||Interstellar and circumstellar matter|
|Published online||15 March 2001|
The circumstellar structure of the Be shell star Persei*
Institut für Astronomie und Astrophysik und Universitäts-Sternwarte München, Scheinerstr. 1, 81679 München, Germany
2 European Southern Observatory, Karl-Schwarzschildstr. 2, 85745 Garching, Germany
3 Astronomical Institute, Academy of Sciences of the Czech Republic, 25165 Ondřejov
Corresponding author: W. Hummel, firstname.lastname@example.org
Accepted: 12 December 2000
We model Feii 5317 emission lines and phase resolved Hei 6678 and 5876 emission lines of the bright B2e& sdO shell binary ϕ Per to find the size and shape of the excitation region inside the circumprimary disk. We find the Feii 5317 emission to originate within 9 stellar radii in an axisymmetric disk around the primary. Orbital phase variations of Hei 6678 are fit in terms of a disk sector with disk radius of 10 stellar radii and opening angle of facing the secondary. This region can be alternatively described by an intersection of a sphere around the secondary and the circumprimary disk with a penetration depth of about . Similar fit values are found for Hei 5876. The enigmatic orbital phase precedence of shell occurrence in the Hei emission features is discussed. We favor a model in which the inner Hei shell is deformed because of differential rotation in combination with a finite recombination time.
Key words: line: formation, profiles stars: circumstellar matter, emission-line, Be, binaries, spectroscopic
Based on observations collected at the Ondřejov Observatory (of the Academy of Sciences of the Czech Republic), the German-Spanish Astronomical Center (DSAZ) -Calar Alto (operated by the Max-Plank-Institut für Astronomie Heidelberg jointly with the Spanish National Commission for Astronomy) and Observatoire de Haute-Provence (OHP; CNRS, France).
© ESO, 2001
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