Classification of magnetospheric responses to interaction with diamagnetic structures of slow solar wind

Parkhomov, V. A.; Еселевич, В. Г.; Еселевич, М.; Дмитриев, А. В.; Suvorova, A. V.; Vedernikova, Tatyana

doi:10.12737/szf-64202004

Solnechno-Zemnaya Fizika

2020

DOI: 10.12737/szf-64202004

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Classification of magnetospheric responses to interaction with diamagnetic structures of slow solar wind

V. A. Parkhomov

В. Г. Еселевич

М. Еселевич

et al.

Abstract: We propose a possible classification of the responses of the magnetosphere to the interaction with diamagnetic structures (DS), which form the basis of the slow solar wind. The main determinants of the classification are the value and orientation of the vertical component Bz of the interplanetary magnetic field (IMF) and the solar wind density N. We have identified three types of magnetospheric responses. Type 1 has two subtypes whose main difference is the presence or absence of auroras on the day side of the… Show more

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Cited by 2 publications

References 27 publications

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

Parkhomov

Еселевич

et al. 2021

Solnechno-Zemnaya Fizika

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

Parkhomov

Еселевич

et al. 2021

Solnechno-Zemnaya Fizika

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Correspondence of a global isolated substorm to the McPherron statistical model

Parhomov

Еселевич

et al. 2022

Solnechno-Zemnaya Fizika

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It is shown that a diamagnetic structure (DS) of the slow solar wind (SW), the source of which on the Sun was a chain of streamers, arrived at Earth’s orbit on December 22, 2015. It interacted with Earth’s magnetosphere under conditions when the northward Bz component of the interplanetary magnetic field (IMF) remained for a long time in preceding undisturbed SW. The interaction and a sharp change in the direction of Bz to the south generated an isolated substorm whose duration depends on the duration of interaction with the DS. The substorm began at midday with the passage of the DS into the magnetosphere and spread to the east. All phases of the substorm — growth, expansion, and recovery — were observed for two hours. Variations in the SW and IMF parameters are shown to coincide for the isolated substorm whose energy source was the slow solar wind DS, and a trigger was the abrupt change in the direction of the vertical IMF component from north to south. The coincidence is justified by statistical generalizations of the same parameters in 40 % of cases of long-term observations of individual substorms whose trigger was a change in Bz direction.

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Classification of magnetospheric responses to interaction with diamagnetic structures of slow solar wind

Cited by 2 publications

References 27 publications

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

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

Correspondence of a global isolated substorm to the McPherron statistical model

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