Draping of strongly flow-aligned interplanetary magnetic field about the magnetopause

Petrinec, S. M.

doi:10.1016/j.asr.2015.10.001

Cited by 11 publications

(11 citation statements)

References 22 publications

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“…However, a draping effect would turn the earthward IMF into the dawnward magnetosheath magnetic field at the THEMIS‐D location, but the duskward orientation was observed. This opposite than the expected B y sign was already pointed out by Petrinec () for intervals of a nearly radial IMF but without any interpretation. We think that the reversal of the B y sign can be connected with component reconnection at the high‐latitude magnetopause, and thus, the region IV would be also a part of the MSBL.…”

Section: Observations Of Boundary Layersmentioning

confidence: 61%

Formation of the Dayside Magnetopause and Its Boundary Layers Under the Radial IMF

Němeček

Šafránková

et al. 2018

JGR Space Physics

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The global structure of magnetopause boundary layers under the radial interplanetary magnetic field (IMF) conditions is studied by a comparison of experimental and simulation results. In magnetohydrodynamic simulations, the hemispherical asymmetry of the reconnection locations was found. The draped field adjacent to the magnetopause points northward in the Northern Hemisphere, but it is oriented southward in the Southern Hemisphere at the beginning of the simulation for negative IMF B x . The magnetopause region affected by the positive IMF B z component enlarges over time, and the density profile exhibit a north-south asymmetry near the magnetopause. The experimental part of the study uses the Time History of Events and Macroscale Interactions during Substorm data. We analyze profiles of the plasma parameters and magnetic field as well as the ion pitch-angle distributions. The nonsimultaneous appearance of parallel and antiparallel aligned flows suggests two spatially separated sources of these flows. We have identified (1) the inner part of the low-latitude boundary layer (LLBL) on closed magnetic field lines; (2) the outer LLBL on open field lines; (3) the inner part of the magnetosheath boundary layer (MSBL) formed by dayside reconnection in the Southern Hemisphere; and (4) the outer MSBL resulting from lobe reconnection in the Northern Hemisphere.

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Section: Observations Of Boundary Layersmentioning

confidence: 61%

Formation of the Dayside Magnetopause and Its Boundary Layers Under the Radial IMF

Němeček

Šafránková

et al. 2018

JGR Space Physics

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“…The draped field is also seen in their results. Similarly, Petrinec [] reported the draped field occurring rather far downstream of the bow shock under the radial IMF conditions.…”

Section: Introductionmentioning

confidence: 99%

“…The draped field is also seen in their results. Similarly, Petrinec [2016] reported the draped field occurring rather far downstream of the bow shock under the radial IMF conditions. Dayside reconnection is one of the major mechanisms that govern the global magnetic field structure near the magnetopause.…”

Section: Introductionmentioning

confidence: 99%

Evolution of the magnetic field structure outside the magnetopause under radial IMF conditions

Shue

Grygorov

et al. 2017

JGR Space Physics

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We use the Time History of Events and Macroscale Interactions during Substorms data to investigate the magnetic field structure just outside the magnetopause and its time evolution for radial interplanetary magnetic field (IMF) events. When the magnetic field drapes around the magnetopause in the magnetosheath region, an asymmetric magnetic field orientation in different hemispheres is expected. Our two‐case study reveals some conflicts with the predicted draped field configuration in the Southern Hemisphere. The magnetosheath Bz component had a different sign depending on the upstream IMF Bx component's polarity at the beginning of the radial IMF intervals. With time, the observed Bz became northward in both cases with increasing positive values through the events. The increasing value of the Bz component may be explained by two possible mechanisms: by a change of the upstream IMF and by a reconnection between magnetosheath and magnetospheric field lines. Our study shows that both mechanisms contributed to the observed changes. Thus, there was a correlation between the change of the upstream IMF conditions and an increase in the magnetosheath northward magnetic field component. The observed formation of the boundary layer near the magnetopause proves that the reconnection process was ongoing at least for a part of the time. We suggest two possible reconnection scenarios: one near subsolar point and another tailward of the one cusp due to lobe reconnection. The asymmetry of reconnection locations causes rearrangement of the magnetic field structure near the magnetopause and turns the observed magnetosheath Bz component even further into positive values.

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“…The additional positive cell in the dayside polar cap (Figures 4a and 4c) implies that the single lobe reconnection site is displaced toward the dawn sector from the noon-midnight meridian. According to Petrinec (2016), the location where the draped IMF lines diverge moves further downstream with respect to the location at which the IMF is parallel to the magnetopause normal, when the IMF is not perfectly aligned with the solar wind flow. This location can be placed on the dusk side of the magnetopause under negative IMF B x and negative IMF B y conditions.…”

Section: Discussionmentioning

confidence: 99%

Radial Interplanetary Magnetic Field‐Induced North‐South Asymmetry in the Solar Wind‐Magnetosphere‐Ionosphere Coupling: A Case Study

et al. 2022

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The paradigm that magnetospheric convection is driven by the process of magnetic reconnection between the interplanetary magnetic field (IMF) and terrestrial magnetic field was first proposed by Dungey (1961). Following this seminal work, enormous attention has been paid to the influence of the IMF orientation on the solar wind-magnetosphere interaction and its influence on the large-scale plasma convection in the high-latitude (polar and auroral) ionosphere (Milan & Grocott, 2021, and references therein). Previous studies pointed out that among three components of the IMF in geocentric solar magnetospheric (GSM) coordinates, the north-south (vertical) component (that is, IMF B z ) largely determines the global convection pattern of the plasma in the high-latitude ionosphere of both the Northern and Southern Hemispheres. Specifically, this consists of two vortex cells with an anti-sunward flow across the polar cap and a sunward return flow at lower latitudes in the morning and evening sectors (a two-cell convection pattern) under purely southward IMF conditions. When IMF is northward, on the other hand, two additional cells with reversed vorticity (a four-cell convection pattern) can exist in the central polar cap. These convection cells are observed to be significantly distorted toward either the dawn or dusk sector depending on the sign of dawn-dusk (azimuthal) IMF component (IMF B y ) (Heppner & Maynard, 1987). The convection pattern essentially shows a mirrored symmetry with respect to the noon-midnight meridian between the hemispheres.Compared to these two IMF components, less attention has been paid to the influence of the Sun-Earth (radial) IMF component (IMF B x ) on the solar wind-magnetosphere-ionosphere (SW-M-I) coupling. This is because its

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Draping of strongly flow-aligned interplanetary magnetic field about the magnetopause

Cited by 11 publications

References 22 publications

Formation of the Dayside Magnetopause and Its Boundary Layers Under the Radial IMF

Formation of the Dayside Magnetopause and Its Boundary Layers Under the Radial IMF

Evolution of the magnetic field structure outside the magnetopause under radial IMF conditions

Radial Interplanetary Magnetic Field‐Induced North‐South Asymmetry in the Solar Wind‐Magnetosphere‐Ionosphere Coupling: A Case Study

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