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

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

doi:10.12737/szf-54201905

Cited by 3 publications

(3 citation statements)

References 14 publications

(28 reference statements)

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“…In a recent study, Parkhomov et al. (2019) using OMNI solar wind data identified structures that were likely the solar wind counterpart of the magnetosheath diamagnetic plasmoids measured by Cluster, thus supporting the scenario in which magnetic holes can enter the magnetosheath. Once in the magnetosheath, their increased momentum due to their higher density may affect the magnetosphere in similar way as magnetosheath jets (Plaschke, Hietala, et al., 2018), for example, triggering surface waves, reconnection and impulsive penetration.…”

Section: Introductionmentioning

confidence: 78%

Magnetic Holes in the Solar Wind and Magnetosheath Near Mercury

et al. 2021

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Solar wind magnetic holes were first reported by Turner et al. (1977) using magnetic field data from the Explorer 43 (IMP-6) spacecraft, and were defined as "isolated regions in the form of distinct depressions, or 'holes' in otherwise nearly average conditions." Such magnetic holes have since then been studied by many authors, at various heliocentric distances. We stress here that we will use the original definition of Turner et al. (1977) that the magnetic holes be isolated, and not a part of a quasi-periodic train as seen in observations of mirror mode waves (e.g.,

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Section: Introductionmentioning

confidence: 78%

Magnetic Holes in the Solar Wind and Magnetosheath Near Mercury

et al. 2021

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“…In another study, Madanian et al (2022) showed evidence for crossing of the bow shock by a large-scale upstream magnetic hole by analyzing data from several spacecraft. Finally, Parkhomov et al (2019) reported on a structure observed in the solar wind that shows considerable similarities to a magnetosheath diamagnetic plasmoid from the observations of Karlsson et al (2015), with the solar wind observations made about 90 s earlier then the magnetosheath one.…”

Section: Introductionmentioning

confidence: 88%

“…Sperveslage et al, 2000;Winterhalter et al, 1994) or mirror mode structures created when the plasma is marginally mirror unstable (Karlsson et al, 2021a). Other theories are that the magnetic holes are the result of non-linear interaction of Alfvén waves with the solar wind plasma (Buti et al, 2001;Tsurutani et al, 2002a, b), emerging coherent structures in solar wind turbulence (Perrone et al, 2016;Roytershteyn et al, 2015), or diamagnetic structures formed in the solar corona (Parkhomov et al, 2019).…”

Section: Introductionmentioning

confidence: 99%

Solar wind magnetic holes can cross the bow shock and enter the magnetosheath

Karlsson

Trollvik

Raptis

et al. 2022

Preprint

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Abstract. Solar wind magnetic holes are localized depressions of the magnetic field strength, on time scales of seconds to minutes. We use Cluster multipoint measurements to identify 26 magnetic holes which are observed just upstream of the bow shock and, a short time later, downstream in the magnetosheath, thus showing that they can penetrate the bow shock and enter the magnetosheath. For two magnetic holes we show that the relation between upstream and downstream properties of the magnetic holes are well described by the MHD Rankine-Hugoniot jump conditions. We also present a small statistical investigation of the correlation between upstream and downstream observations of some properties of the magnetic holes. The temporal scale size, and magnetic field rotation across the magnetic holes are very similar for the upstream and downstream observations, while the depth of the magnetic holes varies more. The results are consistent with the interpretation that magnetic holes in Earth's and Mercury's magnetosheath are of solar wind origin, as has previously been suggested. Since the solar wind magnetic holes can enter the magnetosheath, they may also interact with the magnetopause, representing a new type of localised solar wind-magnetosphere interaction.

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

Parkhomov

Еселевич

et al. 2020

Solnechno-Zemnaya Fizika

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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 magnetosphere. Within an hour before DS arrival, Bz has a positive value (up to 12 nT) or fluctuates about 0 in the range from –1 to +1 nT. For both subtypes, the duration of substorm disturbances approximately coincides with the duration of DS, and their intensity does not exceed AE~500 nT. Type 2 is characterized by the fact that before the contact with DS positive IMF Bz (0–10 nT) is recorded for an hour, and at the interface of DS a rapid (≤2 min) change in the orientation of the IMF vertical component from north to south occurs. For type 3, Bz within an hour before the contact with DS is negative (from –10 to 0 nT). We address the problem of DS energy transfer to the magnetosphere.

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

Cited by 3 publications

References 14 publications

Magnetic Holes in the Solar Wind and Magnetosheath Near Mercury

Magnetic Holes in the Solar Wind and Magnetosheath Near Mercury

Solar wind magnetic holes can cross the bow shock and enter the magnetosheath

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

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