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Astron. Astrophys. 321, 867-876 (1997)


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A study of the infrared spectrum of [FORMULA] Persei

I. A parameter study of the disc model

J.M. Marlborough 1, J.-W. Zijlstra 2 and L.B.F.M. Waters 3, 4

1 Department of Physics and Astronomy, The University of Western Ontario, London, Ontario N6A 3K7, Canada
2 Kapteyn Astronomical Institute, P.O. Box 800, 9700 AV Groningen, The Netherlands
3 Astronomical Institute Anton Pannekoek, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
4 SRON Laboratory for Space Research Groningen, P.O. Box 800, 9700 AV Groningen, The Netherlands

Received 22 August 1996 / Accepted 18 November 1996

Abstract

We report a parameter study of emission lines arising from a disc surrounding a Be star, using parameters appropriate to the Be star [FORMULA] Per. We concentrate on the H [FORMULA] line and on some IR recombination lines (Br [FORMULA], Br [FORMULA], Pf [FORMULA] and HI 17-6). The model we use is a simple cone-like disc model, first proposed by Waters (1986). This model has been successful in explaining the continuum energy distribution of Be stars, and we now wish to study the emission line spectrum emerging from such a disc. We find that line shapes and ratios of line strengths are strongly dependent on the temperature structure of the disc. Infrared recombination lines will therefore be very useful in determining the physical state of the circumstellar envelopes of Be stars.

Key words: stars: Per; circumstellar matter; emission-line, Be – infrared: stars

Send offprint requests to: J.M. Marlborough

© European Southern Observatory (ESO) 1997

Online publication: June 30, 1998

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