Resistive instabilities of current sheets in the solar wind

Details Resistive instabilities of current sheets in the solar wind Resistive instabilities of current sheets in the solar wind

Apr 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979ncimc...2..127d&link_type=abstract

Nuovo Cimento C, Serie 1, vol. 2C, Mar.-Apr. 1979, p. 127-138.

Astronomy and Astrophysics

Astronomy

Current Sheets, Interplanetary Magnetic Fields, Magnetohydrodynamic Stability, Solar Wind, Spaceborne Astronomy, Eigenvectors, Magnetic Effects, Perturbation Theory, Plasma Conductivity, Propagation Modes

Scientific paper

Resistive magnetohydrodynamic instabilities are investigated numerically for non-antisymmetric magnetic field profiles similar to those indicated in spacecraft data on solar wind discontinuities. The eigenvalue problem derived for the growth rate of possible instabilities from dimensionless equations for velocity and magnetic field perturbations is solved starting from the outer regions where the plasma is frozen to the magnetic field. For an antisymmetric magnetic profile, calculations show only tearing modes to be present, with instabilities occurring only at long wavelengths, while for a non-antisymmetric magnetic profile resembling the observed solar wind, calculations indicate the presence of rippling modes driven by resistivity gradients, in addition to the tearing modes. Calculations of the scale lengths of variation of the reversing component based on a scaling law relating the maximum growth rate to the magnetic Reynolds number are found to agree with observed solar current sheet scale lengths.

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