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Search for optical coronal line emission from the X-ray sources Epsilon Orionis /B0 Ia/ and Kappa Orionis /B0.5 Ia/A search was conducted for evidence of a coronal region at the base of the winds of Epsilon Ori and Kappa Ori, by means of high signal-to-noise observations at the forbidden lines of Fe X, at 6574 A, and Fe XIV, 5303 A. Both stars have been detected as soft X-ray sources, and show anomalously strong O VI lines in their UV spectra. Large coronal emission measures were expected from the total X-ray flux and Auger-enhanced ionization, but the fact that the iron coronal lines were not detected places new limits on the emission measure if the total temperature is in the range of 700,000-3,000,000 or more than 1,000,000 for Kappa Ori and 2,000,000 for Epsilon Ori. It is suggested that at least some of the X-rays arise, not from the base corona, but from source features farther out in the wind.
Document ID
19810064645
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Nordsieck, K. H.
(Wisconsin Univ. Madison, WI, United States)
Cassinelli, J. P.
(Wisconsin Univ. Madison, WI, United States)
Anderson, C. M.
(Washburn Observatory Madison, WI, United States)
Date Acquired
August 11, 2013
Publication Date
September 1, 1981
Publication Information
Publication: Astrophysical Journal
Subject Category
Astronomy
Accession Number
81A49049
Funding Number(s)
CONTRACT_GRANT: NSF AST-77-06977
CONTRACT_GRANT: NAG8-345
Distribution Limits
Public
Copyright
Other

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