An EXOSAT observation of the morphology of the coronal X-ray emission from Algol

Details An EXOSAT observation of the morphology of the coronal X-ray emission from Algol An EXOSAT observation of the morphology of the coronal X-ray emission from Algol

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985ssrv...40...25w&link_type=abstract

(ESA, ESLAB Symposium on X-Ray Astronomy in the EXOSAT Era, 18th, The Hague, Netherlands, Nov. 5-9, 1984) Space Science Reviews

Astronomy and Astrophysics

Astronomy

Cool Stars, Emission Spectra, Exosat Satellite, Spaceborne Astronomy, Stellar Coronas, X Ray Spectra, Iron, Line Spectra, Spectral Energy Distribution, Stellar Flares, Stellar Luminosity, Stellar Spectrophotometry, Stellar Temperature

Scientific paper

The results of 35 hours of continuous observation of X-ray emission from Algol are reported. The observations were carried out using the Low Energy and Medium Energy Experiments on board Exosat during a secondary optical eclipse beginning at 0900 UT in August 1983. The medium energy spectrum had a temperature of 2.5 x 10 to the 7th K, corresponding to the hard component previously observed by the Einstein Observatory. No obvious X-ray eclipse was observed. An X-ray flare was detected with a peak luminosity of 1.4 x 10 to the 31st erg/s and a total duration of eight hours. The peak temperature of the flare was 5.0 keV with an emission measure of 9.4 x 10 to the 53rd per cu cm. The athermal nature of the flare was confirmed by the detection of an iron line with an EW of about 2 keV. The decay time was fitted to a known cooling law yielding an estimate of the size of the flaring loop of about 0.3 stellar radii. It is suggested that the flare occurred in one of the loops responsible for the lower temperature component observed by the Einstein SSS.

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