Quiescent and Flaring Structure in RS Canum Venaticorum Stars

Details Quiescent and Flaring Structure in RS Canum Venaticorum Stars Quiescent and Flaring Structure in RS Canum Venaticorum Stars

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...570..799s&link_type=abstract

The Astrophysical Journal, Volume 570, Issue 2, pp. 799-819.

Astronomy and Astrophysics

Astronomy

44

Stars: Coronae, Stars: Individual: Constellation Name: Σ Geminorum, Stars: Individual: Constellation Name: Ux Arietis, Stars: Individual: Constellation Name: Ii Pegasi, Stars: Individual: Constellation Name: V711 Tauri, Stars: Individual: Constellation Name: Ab Doradus, Stars: Individual: Constellation Name: Β Ceti, Stars: Late-Type, Ultraviolet: Stars, X-Rays: Stars

Scientific paper

Four of the most active RS CVn stars (V711 Tau, II Peg, σ Gem, and UX Ari) have been observed for a total of 3 Ms with the Extreme Ultraviolet Explorer satellite (EUVE) between 1992 and 2000 January. Flaring and quiescent states of extreme ultraviolet spectra (λλ70-740) and light curves (λλ75-175) have been analyzed to provide emission measure distributions (EMD) for these systems in the range logTe(K)~5.6-7.4, based principally on iron lines. Flux measurements obtained with IUE and the Orbiting and Retrievable Far and Extreme Ultraviolet Spectrometer (ORFEUS) complete the EMD in the lower temperature range [logTe(K)~4.0-5.6]. Frequent flaring activity has been found in the systems, including an increase during the rise phase by a factor of ~9 in the flux of σ Gem, the largest flare enhancement observed with EUVE. Analyses of the EUVE emission in the active single star AB Dor and the low-rotation giant star β Cet are also included. The EMDs are remarkably similar among all the stars, showing a narrow enhancement or ``bump'' around logTe(K)~6.9. These narrow bumps are apparently unrelated to rotation rate, spectral type, binarity, or evolutionary stage. Significant material is found at logTe(K)>~7.0 for the most active stars. Modulation of the EUV flux outside of flaring occurs in four of the stars (σ Gem, V711 Tau, UX Ari, AB Dor). The electron density ranges between Ne~1012 and ~1013 cm-3, measured at logTe(K)~7.0, and may reach higher values during flares. These densities and EMD values imply small scale sizes for emitting regions.

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