X-ray and optical observations of a dMe flare star in the T Tauri field

Details X-ray and optical observations of a dMe flare star in the T Tauri field X-ray and optical observations of a dMe flare star in the T Tauri field

Jul 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986mnras.221...77s&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 221, July 1, 1986, p. 77-92.

Astronomy and Astrophysics

Astronomy

7

Flare Stars, M Stars, Stellar Spectra, Stellar Spectrophotometry, Visible Spectrum, X Ray Spectra, Coronal Loops, Electron Density (Concentration), Exosat Satellite, Heao 2, Light Curve, Spaceborne Astronomy, Stellar Luminosity

Scientific paper

The authors present observations of a newly discovered dMe flare star within 20 pc of the Sun. An EXOSAT observation of this source shows an almost complete X-ray flare light curve with rise time ≡600 s, decay time ≡1500 s, and peak luminosity Lx = 6.1×1029erg s-1, a 40-fold increase in brightness over the quiescent level (1.5×1028erg s-1). The total energy in the flare is 2.7×1032 < Ex < 3.3×1033erg. The authors also present results of two Einstein IPC observations. They identify the source with a hitherto unstudied nearby star with magnitude V ≡ 13 and spectral type ≡dM5e, at a distance of ≡13 pc. A loop model for the quiescent corona gives physically unrealistic values for the size of the loop structure; however, considering the quiescent corona to be uniform and symmetrical gives acceptable values for the mean pressure and density. For the flare, the authors explore a variety of different physical assumptions about the cooling mechanism and derive possible values for loop lengths and electron densities.

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