Fast downflows in the solar transition region explained

Details Fast downflows in the solar transition region explained Fast downflows in the solar transition region explained

Jan 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...312..402m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 312, Jan. 1, 1987, p. 402-411.

Astronomy and Astrophysics

Astrophysics

45

Coronal Loops, Magnetohydrodynamic Flow, Solar Atmosphere, Solar Spectra, Stellar Models, Conservation Laws, Doppler Effect, Solar Temperature, Steady Flow, Transition Flow

Scientific paper

Fast downflows observed in the solar transition region are explained in terms of steady flow through loops. The major features of the observed flows - their high speed, persistence over long periods, the predominance of redshifts in emission lines, and the disappearance of Doppler velocities at coronal temperatures - all follow naturally from the model. The dynamic scaling law of Craig and McClymont is used to estimate the degree of heating asymmetry required to drive a given transition region velocity and to investigate the effect of high flow rates on loop pressure. The analytic results are compared with detailed numerical calculations and the influence of gravity and nonuniform loop area is considered.

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