Structures in a non-magnetic solar corona

Details Structures in a non-magnetic solar corona Structures in a non-magnetic solar corona

Sep 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974soph...38..157c&link_type=abstract

Solar Physics, vol. 38, Sept. 1974, p. 157-164.

Physics

Convective Flow, Fine Structure, Flow Stability, Solar Corona, Computer Techniques, Density Distribution, Gas Density, Radial Velocity, Solar Magnetic Field, Solar Wind

Scientific paper

A fluid mechanical convective instability is examined under the conditions found in the solar corona. Linearized density perturbations are shown to grow as they are carried outward by the solar wind. The non-linear instability may be proposed as a cause of coronal structures in nonmagnetic stars, or in regions of the solar corona with weak magnetic fields.

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