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IUE spectra of a flare in the RS Canum Venaticorum-type system UX ArietisIUE spectra of UX Ari obtained during the large flare of 1979 January 1 exhibit chromospheric and transition-region emission-line fluxes about 2.5 and 5.5 times brighter than quiescent fluxes, respectively, and up to 1400 times brighter than the quiet sun. A high-dispersion spectrum of the 2000-3000 A region exhibits enhanced Fe II emission, which is probably associated mainly with the K0 IV star, and enhanced Mg II emission with asymmetric wings extending to +475 km/s. These line wings are interpreted as evidence for mass flow from the K0 IV star to the G5 V star. A speculative scenario of major long-lived RS CVn flares is proposed in which the component stars have very large corotating flux tubes, which occasionally interact. Magnetic reconnection results in flux tubes that temporarily connect the two stars.
Document ID
19800068198
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Simon, T.
(Joint Institute for Laboratory Astrophysics Boulder, Colo., United States)
Linsky, J. L.
(Joint Inst. for Lab. Astrophysics Boulder, CO, United States)
Schiffer, F. H., III
(Computer Sciences Corp. Silver Spring, Md., United States)
Date Acquired
September 4, 2013
Publication Date
August 1, 1980
Publication Information
Publication: Astrophysical Journal
Subject Category
Astronomy
Report/Patent Number
PB81-133506
Accession Number
80A52368
Funding Number(s)
CONTRACT_GRANT: NGL-06-003-057
CONTRACT_GRANT: NAS5-23274
Distribution Limits
Public
Copyright
Other

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