Simulation of earth's radiation during solar proton events in the process of geomagnetic reversal

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The radiation from galactic and solar cosmic rays as they pass through the modern and rarefied (as a result of multiple reversals) atmosphere during solar proton events and at the time of geomagnetic reversal is studied. We assume that during the reversal process the geomagnetic field weakens and takes on an axisymmetric quadrupole configuration. It is shown that in the case of a single reversal, when the atmosphere does not have time to change, radiation dose powers increase only at low latitudes and are identical to the modern radiation at the poles. However, during the period of multiple inversions, when the atmosphere is rarefied, the level of radiation at the moment of reversal on the Earth's surface increases, on average, twice as much as today's radiation at all latitudes, which can affect the biosphere.

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作者简介

N. Levashov

Space Research Institute

编辑信件的主要联系方式.
Email: nn.levashov@physics.msu.ru
俄罗斯联邦, Moscow

O. Tsareva

Space Research Institute

Email: nn.levashov@physics.msu.ru
俄罗斯联邦, Moscow

V. Popov

Space Research Institute; Lomonosov Moscow State University; HSE University

Email: nn.levashov@physics.msu.ru

Физический факультет

俄罗斯联邦, Moscow; Moscow; Moscow

H. Malova

Space Research Institute; Lomonosov Moscow State University

Email: nn.levashov@physics.msu.ru

Научно-исследовательский институт ядерной физики им. Д.В. Скобельцына

俄罗斯联邦, Moscow; Moscow

L. Zelenyi

Space Research Institute

Email: nn.levashov@physics.msu.ru
俄罗斯联邦, Moscow

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2. Fig. 1. Spectra of primary GCR protons (black solid curve), alpha particles (red curve) of GCR during solar minimum and SPE protons (black dotted curve)

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3. Fig. 2. Dependence of temperature (black dotted curve) and pressure (red solid curve) of the modern atmosphere on altitude

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4. Fig. 3. Rigidity of the geomagnetic cutoff of axisymmetric dipole and quadrupole magnetic fields on magnetic latitude

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5. Fig. 4. Power of radiation doses from GCR at an altitude of 10 km for protons (a), neutrons (b), muons (c) and electrons (d)

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6. Fig. 5. Power of radiation doses from GCR on the Earth's surface for muons (a) and neutrons (b)

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7. Fig. 6. Power of total radiation doses from GCR at an altitude of 10 km (a), on the Earth's surface (b)

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8. Fig. 7. Power of radiation doses from SCR during SPE at an altitude of 10 km for protons (a), neutrons (b), electrons (c), total for all particles (d)

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9. Fig. 8. Power of radiation doses from SCR during SPE for neutrons on the Earth's surface

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