The dissipation of shock waves in the outer solar atmosphere - A reappraisal

Details The dissipation of shock waves in the outer solar atmosphere - A reappraisal The dissipation of shock waves in the outer solar atmosphere - A reappraisal

Mar 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...119..321f&link_type=abstract

Astronomy and Astrophysics, vol. 119, no. 2, Mar. 1983, p. 321-323.

Astronomy and Astrophysics

Astrophysics

2

Coronal Holes, Energy Dissipation, Shock Heating, Shock Wave Profiles, Solar Atmosphere, Solar Temperature, Astronomical Models, Entropy, Plasma Heating, Shock Discontinuity, Shock Wave Propagation

Scientific paper

The problem of the dissipation of shock waves in the solar transition region is reconsidered in the light of recent work (Flower and Pineau des Forets, 1981, 1982) on the variations with time of physical conditions behind a shock. Adopting the coronal hole model of Pineau des Forets (1979), it is concluded that shock waves of 300 s period are not significantly dissipated at steady-state temperatures not greater than approximately 400,000 K and may explain the heating of coronal holes. The value of the shock wave flux derived under the assumption of a sawtooth pressure profile, which has often been adopted in previous work, is found to be in good agreement with more accurate calculations reported here.

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