The Kelvin-Helmholtz instability in photospheric flows - Effects of coronal heating and structure

Details The Kelvin-Helmholtz instability in photospheric flows - Effects of coronal heating and structure The Kelvin-Helmholtz instability in photospheric flows - Effects of coronal heating and structure

Feb 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...403..769k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 403, no. 2, p. 769-779.

Astronomy and Astrophysics

Astrophysics

20

Kelvin-Helmholtz Instability, Photosphere, Plasma Heating, Shear Flow, Solar Atmosphere, Solar Corona, Solar Granulation, Solar Magnetic Field, Vortices

Scientific paper

A series of hydrodynamic numerical simulations has been used to investigate the nonlinear evolution of driven, subsonic velocity shears under a range of typical photospheric conditions. These calculations show that typical photospheric flows are susceptible to the Kelvin-Helmholtz instability (KHI), with rapid nonlinear growth times that are approximately half of a typical granule lifetime. The KHI produces vortical structures in intergranule lanes comparable to a typical fluxule radius; this is precisely the correct scale for maximum power transfer to the corona.

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