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Detection of radio continuum emission from ProcyonWe have detected the F5 IV-V star Procyon as a weak and variable 3.6 cm radio continuum source using the VLA. The inferred radio luminosity is similar to, though some-what higher than, the X-band luminosity of the active and flaring sun. The 33 micro-Jy flux density level at which we detected Procyon on four of five occasions is close to the 36 micro-Jy radio flux density expected from a model in which the radio emission consists of two components: optically thick 'stellar disk' emission with a 3.6 cm brightness temperature of 20,000 K that is 50 percent larger than the solar value, and optically thin coronal emission with an emission measure the same as that indicated by Einstein and EXOSAT X-ray flux measurements in 1981 and 1983. The maximum mass-loss rate of a warm stellar wind is less than 2 x 10 exp -11 solar mass/yr. An elevated flux density of 115 micro-Jy observed on a single occasion provides circumstantial evidence for the existence of highly localized magnetic fields on the surface of Procyon.
Document ID
19930046553
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Drake, Stephen A.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Simon, Theodore
(Hawaii Univ. Honolulu, United States)
Brown, Alexander
(Joint Inst. for Lab. Astrophysics Boulder, CO, United States)
Date Acquired
August 16, 2013
Publication Date
March 20, 1993
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 406
Issue: 1
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
93A30550
Funding Number(s)
CONTRACT_GRANT: NASA ORDER W-17772
Distribution Limits
Public
Copyright
Other

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