![]() ![]() Transmitter phase measurements are more difficult to undertake than amplitude. ![]() Normalized linear regression analysis identifies VLF phase as the most important parameter in the regression, followed by solar zenith angle at the midpoint of the propagation path, then the initial solar X‐ray flux level (from 5 min before the impact of the solar flare), with F10.7 cm flux from the day beforehand providing the least important contribution. The use of VLF amplitude observations to determine long or short wavelength X‐ray flux levels have a 4–10 times higher mean square error than when using VLF phase. Linear regression analysis of signals from the NPM transmitter in Hawaii, received at Arrival Heights, Scott Base, Antarctica, over the years 2011–2015 shows that VLF phase perturbations during large solar flares have a 1.5–3 times lower mean square error when modeling the long wavelength X‐ray fluxes than the equivalent short wavelength fluxes. The reliability of the use of VLF phase and amplitude perturbations to determine the X‐ray fluxes involved during 10 large solar flare events (>X1) is examined. A technique for analyzing very low frequency (VLF) radiowave signals is investigated in order to achieve rapid, real‐time detection of large solar flares, through the monitoring of changes in VLF radio signal propagation conditions. ![]()
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