By C. J. Schrijver (auth.), A. Peacock (eds.)
Algol is a triple approach containing a 70 hr eclipsing binary (K IV and B8 V) in a 694 day orbit with an A V superstar. The X-ray emission from the program (Schnopper et al 1976) is believed to be linked to a corona surrounding the lobe filling and synchron ously rotating okay IV celebrity. this is often in line with the similarity of the X-ray spectrum and luminosity of the program to that of the RS CVn binaries which additionally comprise okay sub-giants with related rotation classes and the truth that the luminosity of any coronae surrounding the B8 V and AV spouse stars shouldn't be greater by way of swift rotation (Pallavicini et al 1980, White et al 1980). The Einstein SSS size confirmed the X-ray spectrum to be part with 6 7 temperatures of seven. 10 okay and three. 10 ok (White et al. 1980). As dis stubborn via Swank et al. (1981), the matter in realizing stellar coronae quite often is the best way to scale up the sun version to account for the improved luminosities. The with regards to 900 inclination and comparable sizes for the Band ok stars of three. 6 and three. eight R0 respectively make Algol an awesome candidate for an X-ray eclipse size in which the scale of the X-ray emitting coronal constructions will be at once measured. during this paper we file a continuing remark in the course of the secondary eclipse of Algol utilizing the EXOSAT Observatory. 2.
Read or Download X-Ray Astronomy in the Exosat Era: Proceedings of the XVIII ESLAB Sysmposium, held in The Hague, The Netherlands, 5–9 November 1984 PDF
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