![]() ![]() Multiple time-scale beats in aurora: Precise orchestration via magnetospheric chorus waves. Pulsating aurora from electron scattering by chorus waves. Scattering by chorus waves as the dominant cause of diffuse auroral precipitation. A mechanism of formation of pulsating aurorae. Electron energy measurements in pulsating auroras. Estimation of the emission altitude of pulsating aurora using the five-wavelength photometer. Effective lifetime of O (1 S) in pulsating aurora. Altitude of pulsating aurora determined by a new instrumental technique. Pulsating aurora beyond the ultra-low-frequency range. Multiscale temporal variations of pulsating auroras: On-off pulsation and a few Hz modulation. Differentiating diffuse auroras based on phenomenology. Statistics of pulsating auroras on the basis of all-sky TV data from five stations. On the temporal fluctuations of pulsating auroral luminosity. Pulsating aurora: Local and global morphology. Pulsating Aurora Imaging Photometers Stereoscopic System The following abbreviations are used in this manuscript: The field of view (FOV) of the second photometer is optimized to measure the whole range of possible PsA emission altitudes, placing the high-energy electrons region in the center of the FOV. The profiles of the ionization rate obtained in are shown in the left panel of Figure 1 to compare with proposed geometry of the experiment. The results of both simulations agree with each other and can be used for the primary particle energy reconstructions according to the height profile of the PsA emission. Recently, the Energetic Precipitation Monte Carlo (EPMC) model was developed and employed to calculate the ionization rate as a function of altitude produced by monoenergetic electrons. A detailed simulation of monoenergetic electron beams penetration into the atmosphere was performed in using a SIC (Sodänkyla Ion and Neutral Chemistry) model and the dependence of the ionization rate on energy and height is obtained. The depth of penetration into the gas target is determined by the passed mass and is uniquely found from the initial energy distribution of electrons in the beam by convolution with the dissipation function obtained early by Monte Carlo simulation. Collisional dissipation of energetic electrons in atmospheric gases leads to the generation of a cascade of secondary electrons and rapid isotropization of the electron flux. Energetic electrons of magnetospheric origin rotate while moving along the magnetic field and, according to the configuration of the Earth’s magnetic field, fall into the upper layers at high latitudes. With the help of stereoscopic observations, it is possible to estimate the vertical emission profile, which means that the energy distribution of the precipitated particles (electrons) can be estimated, and the maximum energy of particles in a directed flux from the magnetosphere can be determined. ![]()
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