The circumstellar structure of the Be shell star φ Persei. II. Modeling

Details The circumstellar structure of the Be shell star φ Persei. II. Modeling The circumstellar structure of the Be shell star φ Persei. II. Modeling

Mar 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26a...368..471h&link_type=abstract

Astronomy and Astrophysics, v.368, p.471-483 (2001)

Astronomy and Astrophysics

Astrophysics

12

Line: Formation, Profiles Stars: Circumstellar Matter, Emission-Line, Be, Binaries, Spectroscopic

Scientific paper

We model Fe Ii 5317 emission lines and phase resolved He I 6678 and 5876 emission lines of the bright B2e&sdO shell binary phi Per to find the size and shape of the excitation region inside the circumprimary disk. We find the Fe Ii 5317 emission to originate within 9 stellar radii in an axisymmetric disk around the primary. Orbital phase variations of He I 6678 are fit in terms of a disk sector with disk radius of 10 stellar radii and opening angle of =~ 120degr 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 7 R_*. Similar fit values are found for He I 5876. The enigmatic orbital phase precedence of shell occurrence in the He I emission features is discussed. We favor a model in which the inner He I shell is deformed because of differential rotation in combination with a finite recombination time. 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).

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