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Astron. Astrophys. 358, 208-220 (2000)

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The circumstellar structure of the Be shell star [FORMULA] Per *

I. Data analysis

S. tefl 1, W. Hummel 2 and Th. Rivinius 3,4

1 Astronomical Institute, Academy of Sciences of the Czech Republic, 25165 Ondejov (sstefl@sunstel.asu.cas.cz)
2 Institut für Astronomie und Astrophysik und Universitätssternwarte München, Scheinerstrasse 1, 81673 München, Germany (hummel@bigbang.usm.uni-muenchen.de)
3 European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München (triviniu@eso.org)
4 Landessternwarte Königstuhl, 69117 Heidelberg, Germany

Received 19 February 2000 / Accepted 14 March 2000


We present new phase resolved observations of emission lines of the Be binary [FORMULA] Per.

Analyzing the orbital phase variations in the HeI emission features we find strong arguments that the feature as a whole originates in the outer parts of the disk around the primary star. In addition to the HeI  6678 and 5876 lines, the emission features with orbital phase variations were detected in three more HeI lines. The observations are in agreement with the scenario of Poeckert and others, in which the outer parts of an axisymmetric disk are illuminated by the radiation of the secondary. The observations after 1996 are consistent with a growing global density inhomogeneity in the circumprimary disk as it occurs in disks of single Be stars. The combination of the illumination effect and the increasing density inhomogeneity make [FORMULA] Per an ideal laboratory to study density perturbations of circumstellar disks of Be stars in more detail.

Key words: line: profiles – radiative transfer – stars: binaries: general – stars: circumstellar matter – stars: emission-line, Be – stars: individual: OE Per

* Based on observations collected at the Ondejov Observatory (of the Academy of Sciences of the Czech Republic), Heidelberg Observatory, 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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© European Southern Observatory (ESO) 2000

Online publication: June 26, 2000