11 research outputs found
On stability of rotation of the mean magnetic field of the Sun
New data on the mean magnetic field of the Sun (MMFS) as a star measured
at the Crimean Astrophysical Observatory in 1998–2001 are presented. The
34-year time series of the MMFS using similar data from three other
observatories (1968–2001, with the total number of daily MMFS values N =
12 428), is considered. It is found that (a) the primary synodic period
of the equatorial rotation of solar magnetic field,
 days, did not vary over the last 34 years, but
(b) the average intensity H0 of the photospheric large-scale fields,
by modulus, decreased by about 4.5% (with a confidence level of about
80%). The conclusion is made that the longer, 90-year, cycle might be
responsible for this potential gradual decrease of H0. The average curve of
MMFS variation as plotted with the primary rotational period
demonstrates an obvious N-S asymmetry of polarities, perhaps
associated with the quadrupole component and “magnetic disequilibrium”
of the Sun as a whole