Magnetic activity optimal tracers: from radio to X-ray; the relevance of UV astronomy

Details Magnetic activity optimal tracers: from radio to X-ray; the relevance of UV astronomy Magnetic activity optimal tracers: from radio to X-ray; the relevance of UV astronomy

Apr 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009ap%26ss.320..115p&link_type=abstract

Astrophysics and Space Science, Volume 320, Issue 1-3, pp. 115-120

Astronomy and Astrophysics

Astrophysics

2

Magnetic Activity, Chromospheres, Flare, Late-Type Stars, Solar-Like Winds, Ultraviolet

Scientific paper

Observations and analysis of magnetic activity phenomena in the atmospheres of cool stars—e.g., active regions, flares, stellar cycles—give insight into the fundamental processes in the heating of chromospheres, transition regions (TRs), and coronae. Diagnostics of magnetic activity can be found throughout the whole electromagnetic spectrum; from radio wavelengths, where gyrosynchrotron radiation arises from the quiescent and flaring corona, to optical, where important signatures are the Balmer lines and the Ca ii IRT and H&K lines, eventually to UV and X-rays, the latter mainly due to coronal thermal plasma. The UV and EUV ranges contains a plethora of emission lines that are powerful diagnostics for the warm (10 000 K) chromospheres, hot (100 000-800 000 K) TRs and very hot (1-10 MK) coronae. Also very weak coronal winds from cool stars have been identified and characterized thanks to high resolution UV spectra. Here I review the main results from UV observations of cool stars atmospheres and outline what can be expected from future UV imaging and spectroscopy measurements.

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