Magnetic field and doppler velocity correlation in quiescent solar prominences

Details Magnetic field and doppler velocity correlation in quiescent solar prominences Magnetic field and doppler velocity correlation in quiescent solar prominences

Oct 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996r%26qe...39..857k&link_type=abstract

Radiophysics and Quantum Electronics, Volume 39, Issue 10, pp.857-861

Physics

Scientific paper

Analyzing statistically the magnetic and Doppler velocity data for 85 quiescent prominences observed in 1983 1987 by Nikolsky's magnetograph, we came to the following preliminary conclusions:
The average longitudinal magnetic field of the prominence determines the dynamic velocity of the latter: the stronger magnetic fields correspond to the higher Doppler velocities.
A longitudinal magnetic field less than 25 G allows the material to move with arbitrary velocity within the limits of several kilometers per second. A magnetic field higher than 25 G suppresses such movements.
The horizontal length of the flux tube exceeds its vertical part by 1.5 orders of magnitude (the upper limit).
There is an angle of 10° between the horizontal component of the velocity vector in quiescent prominences and the long axis of the filament.
The maximum velocity in quiescent prominences is about 7 km/s.

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