SpringerLink
Forum Springer Astron. Astrophys.
Forum Whats New Search Orders


Astron. Astrophys. 343, 496-506 (1999)


Table of Contents
Available formats: HTML | PDF | (gzipped) PostScript

An analysis of the incidence of the Vega phenomenon among main-sequence and post main-sequence stars

H. Plets  *  1 and C. Vynckier 2

1 Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, B-3001 Heverlee, Belgium (hansp@oma.be)
2 Departement Wiskunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, B-3001 Heverlee, Belgium (coleet@ibm.net)

Received 16 February 1998 / Accepted 7 December 1998

Abstract

During the past decade, the incidence of the Vega phenomenon has been studied several times statistically, but these studies lack a sufficiently rigorous basis. To improve the discussion, we selected a sample of objects with detectable photospheric fluxes, in casu at 60 µm. Because of the limited sensitivity of IRAS , only a small fraction of the main-sequence stars within 25 parsec from the Sun meet this condition and the sample contains too few objects for a reliable estimation of the fraction of excess stars. We estimate the incidence of the Vega phenomenon by applying robust statistical methods, in casu the Least Median of Squares regression and the Minimum Volume Ellipsoid method, and survival analysis. We find a very similar result for main-sequence stars and their descendants, the first-ascent G-K giants: 13 [FORMULA] 10% of the main-sequence stars show a 60 µm excess and 14 [FORMULA] 5% of the giants.

Key words: methods: statistical – stars: circumstellar matter – stars: evolution – stars: statistics – infrared: stars

* Current address: Royal Meteorological Institute of Belgium, Ringlaan 3, B-1180 Brussels, Belgium

Send offprint requests to: H. Plets

Correspondence to: hansp@oma.be

© European Southern Observatory (ESO) 1999

Online publication: March 1, 1999

helpdesk.link@springer.de