Photospheric Magnetic Reconnection and Canceling Magnetic Features on the Sun

Details Photospheric Magnetic Reconnection and Canceling Magnetic Features on the Sun Photospheric Magnetic Reconnection and Canceling Magnetic Features on the Sun

Apr 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999apj...515..435l&link_type=abstract

The Astrophysical Journal, Volume 515, Issue 1, pp. 435-440.

Astronomy and Astrophysics

Astronomy

69

Sun: Chromosphere, Sun: Magnetic Fields, Sun: Photosphere

Scientific paper

Parameters describing quasi-steady reconnecting current sheets in the plasma of the solar photosphere and chromosphere are computed using the VAL-C atmospheric model. In particular, the inflow speed for the Sweet-Parker magnetic reconnection is found for a sheet whose width is determined by the density scale height. The resulting speed of several tens of meters per second corresponds closely to the speeds implied by observations of canceling magnetic features on the Sun. This and other arguments support photospheric magnetic reconnection as the cancellation mechanism. The reconnection process should be most efficient around the temperature minimum region about 600 km above the lower photospheric boundary.

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