Abstract
We calculate cosmic ray intensity using the model of the Forbush decrease formation in a magnetic cloud by the electromagnetic mechanism for three events. The properties of the Forbush decrease are determined by solving the Boltzmann kinetic equation without particle scattering. At the initial time, the magnetic cloud has the shape of a torus, for which geometric parameters such as velocity, velocity gradient, cross-sectional area, and angular dimensions are specified. The kinematic model determines the subsequent propagation of the cloud in interplanetary space. The magnetic field properties and the type of helical structure near the Sun are based on the Miller and Turner toroidal model. In interplanetary space, magnetic field components are determined by the frozen-in condition. The model properties of the velocity, velocity gradient, magnetic field components, and characteristics of the Forbush decrease roughly agree with measurements in three events. There are no free parameters in the Forbush decrease formation model.
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Funding
This work is supported by the RF Ministry of Science and Higher Education, and by the Siberian Branch of the Russian Academy of Sciences, project no. FWRS-2021-0012. The authors acknowledge the FD database obtained by IZMIRAN Cosmic Ray Group (http://spaceweather.izmiran.ru/eng/dbs.html), the NMDB database (www.nmdb.eu), OMNIWeb (https://omniweb.gsfc.nasa.gov/form/ dx1.html), the near-Earth interplanetary coronal mass ejection database compiled by I.G. Richardson and H.V. Cane (http://www.srl.caltech.edu/ACE/ASC/DATA/level3/icmetable2.htm) for providing the data.
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Petukhova, A.S., Petukhov, I.S. & Petukhov, S.I. Formation of a Forbush Decrease in a Magnetic Cloud by the Electromagnetic Mechanism. Phys. Atom. Nuclei 86, 1133–1137 (2023). https://doi.org/10.1134/S1063778824010435
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DOI: https://doi.org/10.1134/S1063778824010435