All earlier studies of flux variations are based mostly on observations from measurements performed at locations mendacity on the path of the solar eclipse i.e. the shadow region. 1500 keV. Yet another attention-grabbing factor is that the increment or decrement that we observed were sustained throughout the solar eclipse duration that is from the time of the first contact to the time of the final contact. Therefore, all the explanations and interpretations of outcomes obtained by earlier groups of researchers do not hold in our case. Our experiment is exclusive in the sense that the measurements are accomplished at a place lying on the other aspect of the globe.
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In reference zhang a strong signature of ionospheric bow waves has been identified as whole electron content material (TEC) disturbances over central/jap United States (pipihosa.com) throughout the great American Eclipse 2017. Interestingly they not only found the eclipse bow wave in the ionosphere, they discovered sturdy TEC perturbations that move alongside meridional route and zonal path at supersonic speeds which are too quick to be related to known gravity wave or large-scale touring ionospheric disturbance (LSTID) processes. As a way to observe the bow waves, the atmospheric disturbances attributable to other sources should be minimal. As mentioned of their paper, atmospheric and ionospheric disturbances may be excited by many various sources. In keeping with the information from NOAA’s Geostationary Operational Environmental Satellites (GOES) noaa3 there have been no weather turbulences on 21 August.
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The interplay of the cosmic rays in the ambiance is affected by the weather parameters and photo voltaic actions. × 5.1 cm. The crystal is hermetically sealed inside an aluminium casing of 0.8 mm thickness with a 1 mm thick white reflecting materials positioned between the crystal and the casing. We started our measurements a number of days previous to the photo voltaic eclipse day, and continued the identical for the subsequent few days for good statistics of the background counts and estimation of fluctuations. We have now used a NaI(Tl) detector to detect the gamma rays. For shielding the detector from low energy background radiation, a 1 cm thick lead field has been used.
The variation of cosmic ray flux during solar eclipses have been studied. SCR flux in 1 MeV – 1.5 MeV power range throughout annularity p4 . Reported earlier by a number of teams of researchers bhat . All of them observed a dip in cosmic ray flux through the solar eclipse. 2.Four MeV – 2.7 MeV was reported p1 . In keeping with observations by Bhaskar et al. 2 . In one other experiment carried out by Bhattacharya et al. August 1, 2008 in the energy range 50 keV – 4600 keV p3 . The experiment carried out by Chintalapudi et al.
