| Issue |
A&A
Volume 368, Number 2, March III 2001
|
|
|---|---|---|
| Page(s) | 471 - 483 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361:20000559 | |
| Published online | 15 March 2001 | |
The circumstellar structure of the Be shell star
Persei*
II. Modeling
1
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, whummel@eso.org
Received:
18
May
2000
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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