High-velocity plasma in the transition region of AU Microscopii: Evidence for magnetic reconnection and saturated heating during quiescent and flaring conditions

Details High-velocity plasma in the transition region of AU Microscopii: Evidence for magnetic reconnection and saturated heating during quiescent and flaring conditions High-velocity plasma in the transition region of AU Microscopii: Evidence for magnetic reconnection and saturated heating during quiescent and flaring conditions

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...430..342l&link_type=abstract

The Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 430, no. 1, p. 342-350

Astronomy and Astrophysics

Astronomy

56

Atmospheric Heating, Magnetic Field Reconnection, Space Plasmas, Stellar Flares, Stellar Magnetic Fields, Stellar Spectra, Ultraviolet Astronomy, Astronomical Spectroscopy, Hubble Space Telescope, Line Spectra, Spaceborne Astronomy

Scientific paper

We analyze high-resolution HST spectra of the dMOe flare star AU Mic, including the profiles of the C IV 1548.2 A, 1550.8 A and Si IV 1393.8 A, 1402.8 A lines obtained with the G160M grating of the Goddard High-Resolution Spectrograph. The quiescent profiles of the C IV and Si IV lines are broad, and not simple Gaussians in shape. Flux in the C IV and Si IV lines, for example, can be measured reliably out to about +/- 200 km/s from line center. Each of the C IV and Si IV profiles can be fitted accurately by two Gaussians (one narrow and the other broad) centered on nearly the same wavelength, with the narrower component accounting for roughly 60% ofthe total integrated flux. The narrow components have similar line widths to those observed in solar active and quiet regions. The broad Gaussian components of the AU Mic line profiles are reminiscent of the broad C IV profiles observed in solar transition region explosive events, which are thought to be associated with emerging magnetic flux regions where field reconnection occurs.

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