Computer Science
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008cxo..prop.2523s&link_type=abstract
Chandra proposal ID #10200110
Computer Science
Scientific paper
Whether intermediate-mass stars can generate X-ray emission is a long-standing problem. A shallow convective envelope is present, but in constrast to late-type dynamo-active stars their magnetic fields are geometrically simple and stable. Commonly any observed X-ray emission from intermediate-mass stars is ascribed to unresolved late-type companions. The rapidly osciallating Ap stars (roAp) are a class of cool, pulsating, chemically peculiar magnetic stars that are known to be single. Therefore, they are prime targets for the search for coronae in the presence of large-scale organized fields. For an explanation of the recent evidence of Promethium, all isotopes of which decay within two decades, flares seem to be the most plausible production mechanism.
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