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Astron. Astrophys. 324, L41-L44

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Letter to the Editor

A BeppoSAX observation of the coronal X-ray emission
of the active binary VY Ari

F. Favata1, T. Mineo2, and A. N. Parmar1, and G. Cusumano2

1Astrophysics Division - Space Science Department of ESA, ESTEC, Postbus 299, 2200 AG Noordwijk, The Netherlands
2IFCAI/CNR, Via U. La Malfa 153, I-90146 Palermo, Italy

Received 13 May 1997 / Accepted 3 June 1997


We present a study of the X-ray coronal emission from the active binary VY Ari, using data from both the Low Energy Concentrator Spectrometer (LECS) and the Medium Energy Concentrator Spectrometer (MECS) instruments on-board the X-ray satellite BeppoSAX. Using these instruments, the X-ray spectrum of VY Ari can be studied across two full decades of energy, from 0.1 to 10 keV. The spectrum is well fit, across the whole spectral range, with an optically thin plasma MEKAL model with two discrete temperature components, and with an inferred coronal abundance [Fe/H] FORMULA , corresponding to the average typical value of the photospheric abundance in RS CVn-type binaries.

Key words: Stars: individual: VY Ari; stars: late-type; stars: activity; X-rays: stars

Send offprint requests to: F. Favata (ffavata@astro.estec.esa.nl)

© European Southern Observatory (ESO) 1997