Mathematics
Scientific paper
Nov 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992esasp.348..293a&link_type=abstract
In ESA, Proceedings of the First SOHO Workshop: Coronal Streamers, Coronal Loops, and Coronal and Solar Wind Composition p 293-2
Mathematics
2
Emission Spectra, Extreme Ultraviolet Radiation, Line Spectra, Magnetic Field Reconnection, Solar Corona, Solar Magnetic Field, Solar Wind Velocity, Current Sheets, Mathematical Models, Plasma Temperature, Soho Mission, Space Plasmas
Scientific paper
One of the distinctive features of reconnecting magnetic fields in a current sheet in the solar corona is the presence of plasma outflows, whose velocity depends on the plasma temperature inside the current sheet itself. The outflowing plasma is characterized by a symmetric velocity distribution along the line of sight. Therefore the ultimate observational effect of magnetic reconnection is a nonthermal broadening in the emission spectral lines. If reconnection occurs in a pre-flare active region, an observable nonthermal broadening in the XUV lines formed at a few million degrees is expected. The nonthermal profile of the individual spectral lines observed with SOHO (Solar and Heliospheric Observatory) can be computed as a function of the temperature inside the current sheet.
Antonucci Ester
Somov Boris V.
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