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The X-ray corona of ProcyonX-ray emission from the nearby system Procyon A/B (F5 IV + DF) was detected, using the IPC (Imaging Proportional Counter) on board the Einstein Observatory. Analysis of the X-ray pulse height spectrum suggests that the observed X-ray emission originates in Procyon A rather than in the white dwarf companion Procyon B, since the derived X-ray temperature, log T = 6.2, agrees well with temperatures found for quiescent solar X-ray emission. Modeling Procyon's corona with loops characterized by some apex temperature Tmax and emission length scale L, it is found that Tmax is well constrained, but L, and consequently the filling factor of the X-ray emitting gas, are essentially unconstrained even when EUV emission from the transition region is included in the analysis.
Document ID
19850042212
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Schmitt, J. H. M. M. (Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Harnden, F. R., Jr. (Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Rosner, R. (Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Peres, G. (Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Serio, S. (Harvard-Smithsonian Center for Astrophysics, Cambridge, MA; Osservatorio Astronomico Palermo, Italy)
Date Acquired
August 12, 2013
Publication Date
January 15, 1985
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 288
ISSN: 0004-637X
Subject Category
ASTROPHYSICS
Funding Number(s)
CONTRACT_GRANT: NAGW-112
CONTRACT_GRANT: NAG8-445
CONTRACT_GRANT: NAS8-30751
Distribution Limits
Public
Copyright
Other