On measuring energetic (more than 5 MeV) proton fluxes with “METEOR” satellite type Original Research Article

The solar proton data received from various satellites differ from each other making it difficult for modeling. In present paper the proton fluxes data from the solar flares with the GOES and METEOR detectors comparison and analysis of the possible origin of the differences between these values is carried out. The conditions of observation correspond with open space for both satellites. It is deep polar cap for METEOR and geostationary orbit with R = 6.6 for GOES. The GOES fluxes were recalculated to threshold energy of the METEOR with interpolation and 1 h averaging. The METEOR threshold energy was accepted as 5 MeV (1), 15 MeV (2), 32 MeV (M), 40 MeV (3) and 90 MeV (4). It pays attention to abnormal behavior of the relationship for threshold energy equal to 5 MeV. Value of the factor k1 = JGOES(5 MeV)/JMETEOR(5 MeV) exceed values of the others factors in 2 –2.5 times and there is abnormal dispersion (in comparison with the others factors) fluxes relation. We have done some investigations of K1 dependence on the rigidity of the proton flux spectra in the same time for explanation such behavior of the K1. The persistent regularity of K1 indicates that the most part of the spread in values of K1 is involved with dependence with spectra rigidity. The investigation of the dependence of the threshold energy of the METEOR detector with spectra rigidity of the proton flux was carried out. It results from analysis that large transfer zone from energy with effective area “S” equals zero (E < E1) till energy with effective area “S” equal to one. This is the relation of these energies: E2/E1 = 5 (E1 = 4.2 MeV, E2 = 21 MeV). The presence of such zone means that the detector effective area “S” will be different for proton fluxes with different rigidity. After some mathematical transformations you can get that the proton fluxes (measured with 5 MeV METEOR detector) do not correspond to 5 MeV, but 7 MeV. Correction factor E(γ) increases with γ increase from value 1.40 for γ = 2 to value 2.24 for γ = 6 with central tendency about 2. The proton flux for detector with 5 MeV nominal threshold level must be doubling. It is necessary to do such adjustment for all METEOR data from 1972 year.