THE MOTION OF CA(+) IN THE CHROMOSPHERE AND THE CONNECTION OF MOTION WITH MAGNETIC FIELDS.
SACRAMENTO PEAK OBSERVATORY SUNSPOT N MEX
Pagination or Media Count:
The magnetograph and recorder of radial velocities of the Crimean Astrophysical Observatory were used for measuring the longitudinal magnetic field in line Fe lambda 5250 A and radial velocities and brightness in H3Ca. The radial velocity field above active solar regions in flocculi and in undisturbed chromospheric regions was investigated. The radial velocities were compared with the magnetic field distribution at the photospheric level. It was established that in the chromosphere there are extensive regions, with ascending and descending gas, which extend up to 200,000 km. The motion in these regions has the character of large-scale turbulence. The characteristic scale of the elements is 5000-20,000 km and the life-time approx. 7 hours. The total mean velocity of turbulent elements is 3.6 kmsec. In the undisturbed chromosphere the mean velocity of the ascending gas is -0.96 kmsec and the descending 1.25 kmsec. The area from which there is an upward rise of gas comprises 56 of the whole area of the undisturbed chromosphere. The total flow of the ascending mass is equal to the downwardflow. Inflocculi the mean velocity of ascending gas is -0.97 kmsec and descending 1.7 kmsec. The area with a downward flow of gas is more than three times larger than that with an upward flow. The flow of descending gas exceeds that of the ascending gas by a factor of 4. Author
- Plasma Physics and Magnetohydrodynamics