Magnetic reconnection and energy release on the Sun and solar-like stars

Details Magnetic reconnection and energy release on the Sun and solar-like stars Magnetic reconnection and energy release on the Sun and solar-like stars

Apr 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009iaus..259..191v&link_type=abstract

Cosmic Magnetic Fields: From Planets, to Stars and Galaxies, Proceedings of the International Astronomical Union, IAU Symposium,

Astronomy and Astrophysics

Astronomy

Sun: Flares, Sun: Magnetic Fields, Stars: Activity, Stars: Flare, Stars: Magnetic Fields

Scientific paper

Magnetic reconnection is thought to play an important role in liberating free energy stored in stressed magnetic fields. The consequences vary from undetectable nanoflares to huge flares, which have signatures over a wide wavelength range, depending on e.g. magnetic topology, free energy content, total flux, and magnetic flux density of the structures involved. Events of small energy release, which are thought to be the most numerous, are one of the key factors in the existence of a hot corona in the Sun and solar-like stars. The majority of large flares are ejective, i.e. involve the expulsion of large quantities of mass and magnetic field from the star. Since magnetic reconnection requires small length-scales, which are well below the spatial resolution limits of even the solar observations, we cannot directly observe magnetic reconnection happening. However, there is a plethora of indirect evidences from X-rays to radio observations of magnetic reconnection. I discuss key observational signatures of flares on the Sun and solar-paradigm stellar flares and describe models emphasizing synergy between observations and theory.

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