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X-Ray Astronomy in the Exosat Era - Proceedings of the XVIII ESLAB Sysmposium, held in The Hague, The Netherlands, 5-9 November 1984 (Paperback, Softcover reprint of the original 1st ed. 1985)
Loot Price: R3,149
Discovery Miles 31 490
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X-Ray Astronomy in the Exosat Era - Proceedings of the XVIII ESLAB Sysmposium, held in The Hague, The Netherlands, 5-9 November 1984 (Paperback, Softcover reprint of the original 1st ed. 1985)
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Algol is a triple system containing a 70 hr eclipsing binary (K IV
and B8 V) in a 694 day orbit with an A V star. The X-ray emission
from this system (Schnopper et al 1976) is thought to be associated
with a corona surrounding the lobe filling and synchron ously
rotating K IV star. This is based on the similarity of the X-ray
spectrum and luminosity of this system to that of the RS CVn
binaries which also contain K sub-giants with similar rotation
periods and the fact that the luminosity of any coronae surrounding
the B8 V and AV companion stars should not be enhanced by rapid
rotation (Pallavicini et al 1980, White et al 1980). The Einstein
SSS measurement showed the X-ray spectrum to be two component with
6 7 temperatures of 7. 10 K and 3. 10 K (White et al. 1980). As dis
cussed by Swank et al. (1981), the problem in understanding stellar
coronae in general is how to scale up the solar model to account
for the enhanced luminosities. The close to 900 inclination and
similar sizes for the Band K stars of 3. 6 and 3. 8 R0 respectively
make Algol an ideal candidate for an X-ray eclipse measurement
wherein the size of the X-ray emitting coronal structures can be
directly measured. In this paper we report a continuous observation
through the secondary eclipse of Algol using the EXOSAT
Observatory. 2."
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