Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 676, Issue 1, Pages L69-L72Publisher
IOP PUBLISHING LTD
DOI: 10.1086/587055
Keywords
stars : activity; stars : coronae; stars : flare; Sun : activity; Sun : corona; Sun : flares
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There is currently no explanation of why the corona has the temperature and density it has. We present a model that explains how the dynamics of magnetic reconnection regulates the conditions in the corona. A bifurcation in magnetic reconnection at a critical state enforces an upper bound on the coronal temperature for a given density. We present observational evidence from 107 flares in 37 Sun-like stars that stellar coronae are near this critical state. The model may be important to self-organized criticality models of the solar corona.
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