a1cos2(
) + a2cos4() grow
from cycle to cycle.The
Differential Rotation of the Red Solar Corona
(Fe X 6374 Å) from 1957–1994
A. G. Tlatov
High-Altitude
Station of the Main Astronomical Observatory, Russian Academy of
Sciences,
P.O. Box 145, Kislovodsk, 357700 Russia
Received July 2, 1996
Abstract—A
series of observations of the intensity of the solar corona in
the Fe X 6374 Å line is analyzed. Theseries primarily includes
data from the Kislovodsk Station, supplemented with data from the
Sacramento Peak and Pic du Midi observatories. The dependence of
the differential rotation velocity on the phase of the
solar-activity cycle is confirmed: at the cycle minimum, the
rotational velocity of the equatorial regions is maximum and the
latitude dependence of the differential rotation velocity
increases. A latitude–time diagram of zones with slow and
fast differential rotation is constructed, on which waves of
deviation of the differential rotation velocity from the mean
values can be traced; the waves travel from the poles to the
equator. In 1965–1995, the mean values of the coefficients a0
, a1 , and a2 in the
expansion w = a0 a1cos2() + a2cos4() grow
from cycle to cycle.
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