The circumstellar structure of the Be shell star phi Per. I. Data analysis

Details The circumstellar structure of the Be shell star phi Per. I. Data analysis The circumstellar structure of the Be shell star phi Per. I. Data analysis

Jun 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26a...358..208s&link_type=abstract

Astronomy and Astrophysics, v.358, p.208-220 (2000)

Astronomy and Astrophysics

Astrophysics

13

Line: Profiles, Radiative Transfer, Stars: Binaries: General, Stars: Circumstellar Matter, Stars: Emission-Line, Be, Stars: Individual: Phi Per

Scientific paper

We present new phase resolved observations of emission lines of the Be binary phi Per. Analyzing the orbital phase variations in the He I 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 He I 6678 and 5876 lines, the emission features with orbital phase variations were detected in three more He I 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 phi Per an ideal laboratory to study density perturbations of circumstellar disks of Be stars in more detail. Based on observations collected at the Ond\v{r}ejov 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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