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Title:
Detection of soft X-rays from Alpha Lyrae and Eta Bootis with an imaging X-ray telescope
Authors:
Topka, K.; Fabricant, D.; Harnden, F. R., Jr.; Gorenstein, P.; Rosner, R.
Affiliation:
AA(Harvard-Smithsonian Center for Astrophysics, Cambridge, Mass.), AB(Harvard-Smithsonian Center for Astrophysics, Cambridge, Mass.), AC(Harvard-Smithsonian Center for Astrophysics, Cambridge, Mass.), AD(Harvard-Smithsonian Center for Astrophysics, Cambridge, Mass.), AE(Harvard-Smithsonian Center for Astrophysics, Cambridge, Mass.)
Publication:
Astrophysical Journal, Part 1, vol. 229, Apr. 15, 1979, p. 661-668. (ApJ Homepage)
Publication Date:
04/1979
Category:
Astronomy
Origin:
STI
NASA/STI Keywords:
Coronas, Early Stars, Ubv Spectra, X Ray Sources, Solar X-Rays, Stellar Luminosity, Stellar Mass Ejection, Stellar Models, Stellar Winds, X Ray Telescopes
DOI:
10.1086/157000
Bibliographic Code:
1979ApJ...229..661T

Abstract

Results are presented for observations of Alpha Lyr (Vega) and Eta Boo with an imaging X-ray telescope during two rocket flights. It is found that Vega and Eta Boo are soft X-ray sources with respective luminosities of approximately 3 x 10 to the 28th erg/s (0.15-0.8 keV) and 1 x 10 to the 29th erg/s (0.15-1.5 keV). Surface X-ray luminosities of about 640,000 erg/sq cm per sec for Vega and 300,000 erg/sq cm per sec for Eta Boo are estimated and shown to fall within the range of solar coronal X-ray emission. It is concluded that in view of the substantially larger surface areas of these stars, the relatively large total soft X-ray luminosity (as compared with that of the sun) can in both cases be understood as resulting from a moderately active corona, although the Vega observation is in severe conflict with simple models for X-ray emission from single main-sequence stars.

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