Stellar Coronae at the Bottom of the Main Sequence: a Multi-Wavelength Study

Details Stellar Coronae at the Bottom of the Main Sequence: a Multi-Wavelength Study Stellar Coronae at the Bottom of the Main Sequence: a Multi-Wavelength Study

Sep 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001cxo..prop..757r&link_type=abstract

Chandra Proposal ID #03200359

Physics

Chandra Proposal Id #03200359

Scientific paper

It is well established that coronal activity dramatically decreases at the bottom of the main sequence. This was expected: the transition near type M2.5 to fully convective interiors gave impetus for the search for a decline in coronal activity. However, most of the decline occurs later than this transition. Even there, X-ray, H-alpha, and radio flaring continues to at least as late as the brown dwarf LP 944-20 (M9.5), and perhaps is the only means of releasing magnetic energy from an apparently still active dynamo. This leaves us with the question: what is supressing the persistent coronal emission, even as the magnetic flares continue? We will address this question by observing low-mass stars from M6 to L6 in X-ray, H-alpha, and radio wavelengths.

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