Physical conditions in the coronal magnetic tubes

Details Physical conditions in the coronal magnetic tubes Physical conditions in the coronal magnetic tubes

Apr 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975sva....18..617l&link_type=abstract

(Astronomicheskii Zhurnal, vol. 51, Sept.-Oct. 1974, p. 1044-1051.) Soviet Astronomy, vol. 18, Mar.-Apr. 1975, p. 617-620. Tran

Astronomy and Astrophysics

Astronomy

Astronomical Models, Magnetohydrodynamic Flow, Solar Corona, Solar Magnetic Field, Solar Prominences, Atmospheric Models, Density Distribution, Lines Of Force, Magnetoacoustic Waves, Pipe Flow, Solar Activity, Solar Temperature, Steady Flow, Velocity Distribution

Scientific paper

Coronal magnetic tubes are capable of conducting steady flows of matter sufficient to generate quiescent prominences according to Pikelner's (1971) siphon theory. The temperature, particle-concentration, and velocity distributions in such a tube are calculated. It is shown that in a tube the temperature is somewhat lower and the density somewhat higher than in the surrounding corona, and that the temperature and density distributions are governed by the energy flux. A simple method for determining the physical parameters of magnetic tubes in the static case is proposed.

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