Coronal Flaring and the Neupert Effect on the Active Binary Sigma GEM

Details Coronal Flaring and the Neupert Effect on the Active Binary Sigma GEM Coronal Flaring and the Neupert Effect on the Active Binary Sigma GEM

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004cxo..prop.1649b&link_type=abstract

Chandra Proposal ID #06200643

Physics

Chandra Proposal Id #06200643

Scientific paper

We propose coordinated HETGS, STIS, and radio (VLA,VLBA,MERLIN,Arecibo) observations of the RS CVn binary Sigma Gem to observe flaring and quiescent coronal emission, test whether the flares show the Neupert effect expected from chomospheric evaporation models, and determine the flare energy budget. HETGS will measure changes in the coronal emission measure, temperature, density, and elemental abundances. Radio continuum emission will provide a proxy for the high energy particles accelerated during magnetic reconnection. STIS Fe XXI spectra will measure the flare dynamical energy losses. Sigma Gem is an ideal target because it is one of the brightest RS CVns in X-rays, single-lined, and flares 40% of the time. Its long duration flares increase the likelihood of tracking flare evolution.

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