Line formation in Be star circumstellar disks Shear broadening, shell absorption, stellar obscuration and rotational parameter

Details Line formation in Be star circumstellar disks Shear broadening, shell absorption, stellar obscuration and rotational parameter Line formation in Be star circumstellar disks Shear broadening, shell absorption, stellar obscuration and rotational parameter

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26a...359.1075h&link_type=abstract

Astronomy and Astrophysics, v.359, p.1075-1084 (2000)

Astronomy and Astrophysics

Astrophysics

39

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

Scientific paper

We improve the theory of Horne & Marsh on shear broadening in accretion disks of CVs and adapt it to Be star circumstellar disks. Stellar obscuration and shell absorption are taken into account in detail. It is shown that shell absorption is already present in those emission lines where the central depression does not drop below the stellar continuum. The model profiles are fitted to observed symmetric Hα net emission lines with low equivalent width. The derived disk radii range from Rd = 5.3 R_* to Rd = 18 R_* and the surface emissivity varies as ~ R-m with 1.6 < m < 3.5. The comparison between model profiles of rotational parameter j>(1)/(2) with the optically thick Hα profile of HR 5440 rules out the range of j>(1)/(2). This can be understood by the lack of velocity shear in the outer disk regions. We conclude that Keplerian rotation (j=(1)/(2)) is a valid approximation. Based on observations collected at 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. Based on observations collected at the Observatoire de Haute-Provence (OHP), CNRS, France.

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