read more
Home arrow Document
   
Subscriber Authentication Point
 
   
Free access article

This article has an erratum: [erratum]

Issue A&A
Volume 368, Number 2, March III 2001
Page(s) 471 - 483
Section Formation, structure and evolution of stars
DOI 10.1051/0004-6361:20000559



A&A 368, 471-483 (2001)
DOI: 10.1051/0004-6361:20000559

The circumstellar structure of the Be shell star $\mathsf{\phi}$ Persei

II. Modeling
W. Hummel1, 2 and S. Stefl3

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 Ondrejov

(Received 18 May 2000 / Accepted 12 December 2000 )

Abstract
We model FeII 5317 emission lines and phase resolved HeI 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 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 $\simeq$ $120\degr$ 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 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

Offprint request: W. Hummel, whummel@eso.org

SIMBAD Objects



© ESO 2001


What is OpenURL?