Streamer Belt and Chains as the Main Sources of Quasi-Stationary Slow Solar Wind

Еселевич, М.; Еселевич, В. Г.; Fujiki, K.

doi:10.1007/s11207-006-0197-z

Cited by 17 publications

(11 citation statements)

References 25 publications

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“…The quasi-stationary slow SW in the absence of sporadic streams in Earth's orbit features a higher plasma density N > (10 ± 2) cm -3 and a relatively low velocity V≈250-450 km/s as compared to the quasistationary fast SW flowing out of coronal holes whose maximum velocity V ≈ 450-800 km/s [Borrini et al, 1981;Eselevich, Fainshtein, 1991, 1992. Sources of the slow SW on the Sun are the streamer belt [Svalgaard, 1974] and chains [Eselevich et al, 1999;Eselevich et al, 2007], or psevdostreamers [Wang, 2007]). The mechanism of occurrence of the slow SW is still unclear.…”

Section: Introductionmentioning

confidence: 99%

Diamagnetic structures as a basis of quasi-stationary slow solar wind

Еселевич¹

2019

Solar-Terrestrial Physics

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The results presented in this review reflect the fundamentals of the modern understanding of the nature of the structure of the slow solar wind (SW) along the entire length from the Sun to the Earth's orbit. It is known that the source of the slow quasi-stationary SW on the Sun is the belt and the chains of coronal streamers The streamer belt encircles the entire Sun as a wave-like surface (skirt), representing a sequence of pairs of rays with increased brightness (plasma density) or two lines of rays located close to each other. Neutral line of the radial component of the solar global magnetic field goes along the belt between the rays of each of these pairs. The streamer belt extends in the heliosphere is as the heliospheric plasma sheet (HPS). Detailed analysis of data from Wind and IMP-8 satellites showed that HPS sections on the Earth orbit are registered as a sequence of diamagnetic tubes with high density plasma and low interplanetary magnetic field. They represent an extension of rays with increased brightness of the streamer belt near the Sun. Their angular size remains the same over the entire way from the Sun to the Earth's orbit. Each HPS diamagnetic tube has a fine internal structure on several scales, or fractality. In other words, diamagnetic tube is a set of nested diamagnetic tubes, whose angular size can vary by almost two orders of magnitude. These sequences of diamagnetic tubes that form the base of slow SW on the Earth's orbit has a more general name — diamagnetic structures (DS). In the final part of this article, a comparative analysis of several events was made, based on the results of this review. He made it possible to find out the morphology and nature of the origin of the new term “diamagnetic plasmoids” SW (local amplifications of plasma density), which appeared in several articles published during 2012–2018. The analysis carried out at the end of this article, for the first time, showed that the diamagnetic plasmoids SW are the small-scale component of the fractal diamagnetic structures of the slow SW, considered in this review.

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Section: Introductionmentioning

confidence: 99%

Diamagnetic structures as a basis of quasi-stationary slow solar wind

Еселевич¹

2019

Solar-Terrestrial Physics

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“…This line was drawn through the Sun center and the center of the CME, O. It passes along the streamer belt or streamer chains [ Eselevich et al , 1999, 2007]; i.e., it is in the region of the quasistationary slow solar wind (SW).…”

Section: Discussionmentioning

confidence: 99%

On formation of a shock wave in front of a coronal mass ejection with velocity exceeding the critical one

Еселевич

2008

Geophysical Research Letters

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[1] It is shown that in front of a coronal mass ejection, having a velocity u lower than the critical u C relative to the surrounding coronal plasma, there is a disturbed region expended along a direction of the CME propagation. The time difference brightness (plasma density) in the disturbed region smoothly decreases to larger distances in front of the CME. A discontinuity forms at u higher than u C in the disturbed region front part in radial distributions of the difference brightness. Since the u C value is close to the local fast-mode MHD velocity, which in corona approximately equal to the Alfven one, the formation of such a discontinuity when u C is exceeded may be identified with the formation of a shock wave. Citation: Eselevich, M. V., and V. G. Eselevich (2008), On formation of a shock wave in front of a coronal mass ejection with velocity exceeding the critical one, Geophys. Res. Lett., 35, L22105,

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“…В отсутствие спорадического СВ квазистационарный СВ может быть двух типов: быстрый и медленный. Источниками медленного квазистационарного СВ на Солнце являются пояс [Svalgaard et al, 1974] и цепочки стримеров Eselevich et al, 1999], или псевдостримеры . На орбите Земли медленный СВ характеризуется относительно небольшой скоростью V≈ 250-450 км/с по сравнению с квазистационарным быстрым СВ, истекающим из корональных дыр, максимальная скорость которого V~450-800 км/с Eselevich, Fainshtein, 1991.…”

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“…Он разделяет области с противоположным направлением радиальной компоненты глобального магнитного поля [Svalgaard et al, 1974]. Это означает, что в основании пояса стримеров расположены арки магнитного поля, составляющие основу шлема стримера, по вершинам которого проходит нейтральная линия (НЛ) радиальной компоненты глобального магнитного поля Солнца [Eselevich et al, 1999]. Структура пояса корональных стримеров выше шлема представляет собой последовательность пар лучей повышенной яркости (концентрации плазмы) или два близко расположенных ряда лучей.…”

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“…Цепочки отличаются от пояса только тем, что разделяют в короне области с открытыми магнитными силовыми линиями, имеющими одинаковую полярность поля. Поэтому рассчитанные в потенциальном приближении структуры магнитного поля в основании цепочек на поверхности Солнца имеют вид двойных арок [Eselevich et al, 1999].…”

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Diamagnetic Plasmoids as Part of Diamagnetic Structures of the Slow Solar Wind and Their Impact on Earth’s Magnetosphere

Parkhomov

Еселевич

et al. 2019

Solnechno-Zemnaya Fizika

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We have shown that diamagnetic structures (DSs), which form the basis of the slow quasi-stationary solar wind (SW), are observed in Earth’s orbit as a sequence of DSs of various scales. The analysis of this phenomenon indicates that diamagnetic plasmoids in SW, whose concept was introduced by Karlsson in 2015, are identical to small-scale DSs. We have found that the impact of a sequence of DSs in the slow SW on Earth’s magnetosphere causes an increase in geomagnetic activity. Isolated DSs generate short-term magnetic disturbances whose duration is approximately equal to the DS duration. Hence, a sequence of DSs can cause sawtooth substorms. We emphasize that the interaction of DS in the slow SW under northward interplanetary magnetic field can be associated with penetration of DS high-density plasma into the magnetosphere.

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Streamer Belt and Chains as the Main Sources of Quasi-Stationary Slow Solar Wind

Cited by 17 publications

References 25 publications

Diamagnetic structures as a basis of quasi-stationary slow solar wind

Diamagnetic structures as a basis of quasi-stationary slow solar wind

On formation of a shock wave in front of a coronal mass ejection with velocity exceeding the critical one

Diamagnetic Plasmoids as Part of Diamagnetic Structures of the Slow Solar Wind and Their Impact on Earth’s Magnetosphere

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