Influence of processes on the Sun and in the interplanetary medium on the solar proton event on March 30, 2022

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Аннотация

The results of a comparative analysis of the solar proton event on March 30, 2022, which has an unusual time profile of solar proton fluxes, with the previous and subsequent solar proton events (March 28, 2022 and April 02, 2022) are presented. Increases in energetic proton fluxes in interplanetary and near-Earth space are associated with successive solar X-ray flares M4.0, X1.3 and M3.9 and three halo-type coronal mass ejections. The work was done based on experimental data obtained from spacecraft located in interplanetary space (ACE, WIND, STEREO A, DSCOVR), in a circular polar orbit at an altitude of 850 km (Meteor-M2) and in geostationary orbit (GOES-16, Electro-L2). An explanation has been proposed for the features of the energetic proton flux profile in the solar proton event on March 30, 2022: protons accelerated in the flare on March 30, 2022 were partially screened by an interplanetary coronal mass ejection, the source of which was the explosive processes on the Sun on March 28, 2022; late registration of maximum proton fluxes, simultaneous for particles of different energies, is due to the arrival of particle fluxes inside an interplanetary coronal mass ejection. The spatial distribution of solar protons in near-Earth orbit was similar to the distribution at the Lagrange point L1, but with a delay of ~50 min.

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Авторлар туралы

N. Vlasova

Skobeltsyn Institute of Nuclear Physics, Moscow State University

Хат алмасуға жауапты Автор.
Email: nav19iv@gmail.com
Ресей, Moscow

G. Bazilevskaya

Lebedev Physical Institute, Russian Academy of Sciences

Email: nav19iv@gmail.com
Ресей, Moscow

E. Ginzburg

Fedorov Institute of Applied Geophysics

Email: nav19iv@gmail.com
Ресей, Moscow

E. Daibog

Skobeltsyn Institute of Nuclear Physics, Moscow State University

Email: nav19iv@gmail.com
Ресей, Moscow

V. Kalegaev

Skobeltsyn Institute of Nuclear Physics, Moscow State University; Lomonosov Moscow State University

Email: nav19iv@gmail.com

Faculty of Physics

Ресей, Moscow; Moscow

K. Kaportseva

Skobeltsyn Institute of Nuclear Physics, Moscow State University; Lomonosov Moscow State University

Email: nav19iv@gmail.com

Faculty of Physics

Ресей, Moscow; Moscow

Yu. Logachev

Skobeltsyn Institute of Nuclear Physics

Email: nav19iv@gmail.com
Ресей, Moscow

I. Myagkova

Skobeltsyn Institute of Nuclear Physics

Email: nav19iv@gmail.com
Ресей, Moscow

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2. Fig. 1. Time profiles of 03/27/2022−04/05/2022: (a) − Solar X−ray flux densities with a wavelength of 0.1−0.8 nm and (b) - solar proton fluxes according to GOES−16 satellite data, (c) − solar wind velocity and density and (d) - modulus and Bx-MMP components according to the DSCOVR spacecraft.

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3. Fig. 2. Time profiles of solar proton fluxes on 03/27/2022−04/05/2022: (a) with E > 10 MeV and E > 30 MeV according to the ACE spacecraft; (b) with E = 10-160 MeV according to the Meteor-M2 satellite; (c) with E = 9-20 MeV and E = 20-40 MeV according to the Electro-L2 satellite.

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4. Fig. 3. Time profiles of proton fluxes according to the GOES-16 satellite: (a) from 11:00 UT on 03/28/2022 to 11:00 UT on 03/29/2022, (b) from 17:00 UT on 03/30/2022 to 17:00 UT on 03/31/2022, (c) from 13:0000 UT 04/02/2022 to 13:00 UT 04/03/2022

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5. Fig. 4. (a) − Time profiles of proton fluxes with E = 28-72 MeV according to the WIND spacecraft and with E = 40-60 MeV of the STEREO A spacecraft from 03/27/2022 to 04/01/2022 (b) − The layout of the STEREO A spacecraft and the Earth on 30.03.2022 (https://solar-mach .github.io/).

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6. Fig. 5. Time profiles from 16:00 UT on 03/30/2022 to 14:00 UT on 04/01/2022: (a) − solar wind velocity and density according to the DSCOVR spacecraft; (b) − modules B and Bx and (c) − By- and Bz-components of the MMP according to the DSCOVR spacecraft; fluxes of solar protons with energies >10 and >30 MeV according to data from (g) the ACE spacecraft and (e) the GOES-16 satellite.

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7. Fig. 6. Time profiles of the exponent of the power-law energy spectrum of proton fluxes (upper curve) and proton fluxes with E > 10, 60 and 100 MeV according to the GOES–16 satellite 30-31.03.2022: 1 - the beginning of an increase in the proton flux >10 MeV, 2 − >60 MeV, 3 – the arrival the shock front.

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