Bridging the dMe Gap with Ross 154

Details Bridging the dMe Gap with Ross 154 Bridging the dMe Gap with Ross 154

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008xmm..prop...49w&link_type=abstract

XMM-Newton Proposal ID #06019501

Other

Stars, White Dwarfs, Solar System, Ross 154

Scientific paper

M dwarf flare (dMe) stars provide excellent laboratories for the study of magnetic flaring activity, coronal heating, and chemical fractionation mechanisms. Quiescent element abundances seem to be tied to the first ionization potential (FIP), but the nature of that dependence varies with the stellar activity level, whether the emission is quiescent or flaring, and other factors. Understanding flare abundances is important because much of coronal `quiescent' emission is likely the result of continuous X-class `microflares'. Only eight late-type dMe systems have been studied using XMM or Chandra gratings, and a large gap exists between low- and high-activity versions of those stars that can only be bridged with an observation of Ross 154.

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