FLAYERS IN THE PLANETS ATMOSPHERE

Abstract

Planets of the Solar System or exoplanets with atmospheres are complicated to investigate because of the absence of sufficiently intense energy fluxes reflected by their atmospheres. At a sufficiently high brightness of the neighboring star, the atmosphere of the exoplanet gives the absorption spectra of some molecules with a high dissociation potential. If the star's surface temperature is low enough and its activity is low, then the presence of thunderstorm activity in the planet's atmosphere can make it possible to identify it. We show the processes that lead to the formation of flare spectra in the γ- and optical ranges and ways to identify them. It is important to note that current discharges initiate intense nuclear transformations with the formation of proton-rich C11, N13, and O15 nuclei. The spectrum of such a medium is specific and different from the spectra formed by the neighboring star. The statistical irregularity of the frequency of thunderstorms and the variety of conditions in the atmospheres of planets makes it possible to study them due to their illumination in the optical part of the spectrum. It is shown that the integrated optical flow and the detailed γ-spectrum make it possible to trace the time evolution of the lightning head current cord and obtain quantitative values of the current strength. Such fluctuations of the current give changes in the magnetic field of the filament, comparable with the value and even greater than the intrinsic magnetic fields of the planets. To carry out the proposed research, M. Doikov developed a multichannel spectrograph consisting of a γ- and optical spectrometer, a highly sensitive magnetometer, and a radio wave recorder. Its design is discussed in his report. We also note here that the calculations make it possible to determine the statistical parameter of time signals, the operating modes of the equipment, and the selection of the necessary nodes for designing the final working layout of the multichannel spectrometer. The value of the choice of observation site is indicated. In mountainous areas, these are heights of the order of a kilometer. In this case, the devices are near lightning.