Sentence examples for minimum epoch of from inspiring English sources

To reach a compatibility of the theoretical modeling with observations for the last minimum epoch of solar activity 2007 2009 (A < 0) a parallel diffusion coefficient was increased by ∼40%.

We study the 27-day variations of the solar wind velocity, galactic cosmic ray (GCR) intensity and anisotropy in the last minimum epoch of solar activity (2007 2009, A < 0).

However, the periodicity of 7 days is reliably revealed in other parameters characterizing galactic cosmic rays, SW, solar and geomagnetic activities, especially for the minimum epoch of solar activity.

This dependence is stronger in the maximum epoch than in the minimum epoch of solar activity, and is provided by the essential temporal rearrangements of the structure of the Interplanetary Magnetic Field (IMF) turbulence from the maxima to minima epoch of solar activity.

The exponents νy and νz of the power spectral density of the By and Bz components of the IMF in the region of the frequencies (10−6– 4 × 10−6) Hz are larger for the minimum epoch of 1987 (νy ≈ 2.0 and νz ≈ 1.93) than for the maximum epoch of 1990 (νy ≈ 1.43 and νz ≈ 1.27).

The average amplitude of the 27-day variation of the galactic cosmic ray anisotropy (A27A) in the current minimum epoch of solar activity (2007 2009, A < 0) is lesser than in previous positive polarity period as it is expected from the drift theory.

It is suggested that the cycle-to-cycle decrease of the CR density in the minimum epochs of the past solar activity (SA) cycles could be explained by the decrease of the zone-odd index.

We show that the rigidity spectrum of the long-period variations of the GCR intensity is hard in the minimum epochs of solar activity (γ ≈ 0.6) when the exponent νy of the PSD of the IMF is higher (νy ≈ 1.9), and is soft in the maximum epochs (γ ≈ 1.2), when the exponent νy is relatively lower (νy ≈ 1.4).

The dependence of the diffusion coefficient on the cosmic ray particles rigidity R is stronger in the maxima epoch than in the minima epoch of solar activity.

At the same time, during the minima and near minima epochs of solar activity the average amplitudes of the 27-day variations of galactic cosmic rays for neutron monitors are about 1.5 times greater for the qA > 0 cycle than for the qA<0 cycle.

The temporal changes of the energy spectrum of galactic cosmic rays isotropic intensity variations from the maxima to the minima epochs of solar activity indicate the radical redistributions of the EAF's fluctuations (irregularities) from the higher frequencies to the lower frequencies.