University of Oulu

Parhomov V. A., Eselevich V. G., Eselevich M. V., Dmitriev A. V., Suvorova A. V., Khomutov S. Y., Tsegmed B., Tero R. Magnetospheric response to the interaction with the sporadic solar wind diamagnetic structure // Solar-Terrestrial Physics . 2021. no. 3. pp. 11-28. DOI: https://doi.org/10.12737/stp-73202102

Magnetospheric response to the interaction with the sporadic solar wind diamagnetic structure

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Author: Parkhomov, V. A.1; Eselevich, V. G.2; Eselevich, M. V.2;
Organizations: 1Baikal State University, Irkutsk, Russia
2Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
3Lomonosov Moscow State University, Skobeltsyn Institute of Nuclear Physics, Moscow, Russia
4Lomonosov Moscow State University, Moscow, Russia
5Institute of Cosmophysical Research and Radio Wave Propagation FEB RAS, Paratunka, Russia
6Institute of Astronomy and Geophysics AS Mongolia, Ulaan-Baatar, Mongolia
7Sodankyla Geophysical Observatory, University of Oulu, Sodankyla, Finland
Format: article
Version: published version
Access: open
Online Access: PDF Full Text (PDF, 2 MB)
Persistent link: http://urn.fi/urn:nbn:fi-fe2021121460324
Language: English
Published: Infra-M Academic Publishing House, 2021
Publish Date: 2021-12-14
Description:

Abstract

We report the results of a study on the movement of the solar wind diamagnetic structure (DS), which is a sequence of smaller-scale microDS being part of the May 18, 2013 coronal mass ejection, from a source on the Sun to Earth’s surface. DS determined from the high negative correlation coefficient (r=–0.9) between the IMF modulus (B) and the SW density (N) on the ACE and Wind satellites at the L1 point, on the THB and THC satellites (r=–0.9) in near-Earth orbit, and on the THA satellite inside the magnetosphere is carried by the solar wind from the Sun to Earth’s orbit, while maintaining its fine internal structure. Having a large size in the radial direction (≈763 Rᴇ, where Rᴇ is the Earth radius), DS flows around the magnetosphere. At the same time, microDS of size ≤13 Rᴇ passes through the bow shock and magnetopause as a magnetized plasmoid in which the ion concentration increases from 10 cm⁻³ to 90 cm⁻³, and the velocity decreases as it moves toward the magnetotail. When a microDS passes through the magnetopause, a pulsed electric field of ~400 mV/m is generated with subsequent oscillations with a period of T~200 s and an amplitude of ~50 mV/m. The electric field accelerates charged particles of the radiation belt and produces modulated fluxes of protons in an energy range 95–575 keV on the day side and electrons in 40–475 keV and protons in 95–575 keV on the night side. In the duskside magnetosphere (19–23 MLT), the substorm activation is observed in geomagnetic pulsations and auroras, but without a magnetic negative bay. In the post-midnight sector (01–05 MLT), a sawtooth substorm occurs without the growth phase and breakup with deep modulation of the ionospheric current and auroral absorption. The duration of all phenomena in the magnetosphere and on Earth is determined by the period of interaction between DS and the magnetosphere (~4 hrs). To interpret the regularities of the magnetospheric response to the interaction with DS, we consider alternative models of the impulsive passage of DS from SW to the magnetosphere and the classical model of reconnection of IMF and the geomagnetic field.

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Series: Solar-terrestrial physics
ISSN: 2500-0535
ISSN-E: 2500-0535
ISSN-L: 2500-0535
Volume: 3
Issue: 7
Pages: 11 - 28
DOI: 10.12737/stp-73202102
OADOI: https://oadoi.org/10.12737/stp-73202102
Type of Publication: A1 Journal article – refereed
Field of Science: 115 Astronomy and space science
Subjects:
Funding: The work of Parkhomov V.A. was financially supported by the Ministry of Science and Higher Education of the Russian Federation under the project "Development of a mathematical model of the interaction between solar wind diamagnetic structures and Earth's magnetosphere" and by RFBR (Grant No. 18-55-52006 MNTa). The work of Eselevich V.G. and Eselevich M.G. was performed with budgetary funding of Basic Research program II.16. The work of Tsegmed B. was financially supported by the Academy of Sciences of Mongolia (Grant No. SHUAG_2017/17) and by the Ministry of Education, Science and Sports of Mongolia (project No. SHUSS-2017/65). The work of Khomutov S.Yu. was financially supported by the project "Physical processes in the system of near space and geospheres under solar and lithospheric effects", No. АААА-А21-121011290003-0. Measurements with induction magnetometers of the observatories Paratunka and Magadan were carried out within the framework of the agreement on academic exchange between IKIR FEB RAS and the Nagoya Research Institute (Japan) sponsored by the PWING project (JSPS KAKENHI 16H06286).
Copyright information: © 2021 INFRA-M Academic Publishing House (Nauchno-Izdatelskii Tsentr INFRA-M). This is an open access article under the CC BY-NC-ND license.
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