Emergence of magnetic flux from the convection zone into the solar atmosphere. I - Linear and nonlinear adiabatic evolution of the convective-Parker instability

Details Emergence of magnetic flux from the convection zone into the solar atmosphere. I - Linear and nonlinear adiabatic evolution of the convective-Parker instability Emergence of magnetic flux from the convection zone into the solar atmosphere. I - Linear and nonlinear adiabatic evolution of the convective-Parker instability

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apjs...78..267n&link_type=abstract

Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 78, Jan. 1992, p. 267-282. Research supported by Japan Society fo

Astronomy and Astrophysics

Astrophysics

42

Magnetic Flux, Magnetohydrodynamic Stability, Nonlinear Evolution Equations, Photosphere, Solar Atmosphere, Solar Corona, Adiabatic Conditions, Interstellar Matter, Spiral Galaxies

Scientific paper

The linear and nonlinear properties of the evolution of emerging magnetic flux from the solar convection zone into the photosphere, chromosphere, and corona are studied. A linear stability analysis of the partially magnetized convection zone is presented. The growth rate of this combined convective-Parker instability is found to differ significantly from that of the Parker instability in the absence of convection. When beta(=pg/pm) is greater than 10 in the initial flux sheet, the growth rate increases with horizontal wavenumber, and there is no maximum growth rate. A local maximum can occur when the flux is initially located near the top of the convection zone. When beta is less than 10, the convective-Parker instability behaves like the Parker instability for long-wavelength modes, and like the convective instability for short-wavelength modes. A 2D MHD code is used to study the nonlinear evolution of the system. When the initial flux sheet has beta less than 10, the long-wavelength mode dominates the nonlinear evolution of the system, independently of the initial perturbation wavelength.

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