On the consequences of Fisk's type magnetic field configuration for galactic cosmic ray modulation

Three-dimensional steady state transport equation of galactic cosmic rays with drift included is solved by means of newly achieved Fortran code in two cases: 1) Fisk’s type of heliospheric magnetic field dominates in the heliosphere; 2) standard Parker field fills the interplanetary space. The spherically symmetric heliosphere bounded at a distance of 100 AU is assumed. In the calculations the parallel and perpendicular diffusion coefficients are proportional to 1/B, anti-symmetric element of the diffusion tensor has the form derived under the assumption of week-scattering. The computed modulated spectra are presented and compared with experimental data (IMP3, IMP8, balloons, and CAPRICE) for the minimum period of solar activity. The best fit is obtained when the index of the power of rigidity in diffusion coefficient formula is less than 0.8

On the long-term variability of the green corona accordingly to four existing databases

We examine four long-term databases of monthly means of the whole disc green coronal brightness which cover the period of the last five and a half solar cycles to verify them, and compare their usefulness, as indices characterize the solar activity. We use the data from (1) the Norikura Observatory, (2) the Kislovodsk Observatory, (3) intensities detected by several coronographs and converted to the common photometric scale of Pic du Midi, (4) coronal indices obtained from detections of several observatories and converted to the photometric scale of Lomnicky Stit. We compare them by means of correlative analysis with the time series of sunspot numbers. The data (2) demonstrate the best agreement with sunspot number as the reference (r = 0.88)

Secular behaviour of geomagnetic indices IHV, C9, aa since 1901 and presumed rising of solar open magnetic field flux

We examine long-term series of IHV and C9 geomagnetic indices calculated from the data derived during the 20th century in St.-Petersburg, Pavlovsk, Swider, Cheltenham, Fredericksburg, Kakioka, and Honolulu in order to verify the conclusion of Lockwood et al. [8] that the total magnetic flux leaving the Sun increased by a factor of 2.3 since 1901. It was supported on the analysis of aa geomagnetic index which shows a drift upward from the 12th–13th solar cycle to the 22nd cycle. The mean level of the annual averages of indices used here have been approximately constant or showed the clearly smaller rising than aa drift upward from 1901 till 1960. We conclude that the double rising of solar magnetic flux during the 20th century is questionable