Nonlobe Reconnection at the Earth's Magnetopause for Northward IMF

Fuselier, S. A.; Trattner, K. J.; Petrinec, S. M.; Lavraud, B.; Mukherjee, J.

doi:10.1029/2018ja025435

Cited by 11 publications

(17 citation statements)

References 34 publications

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“…The main body of the TPA is in both events associated with BPS-like precipitation, suggesting a formation mechanism on closed field lines. This is in agreement with many previous reports that large-scale TPAs appear commonly in the boundary region reconnection, which has been suggested to be a common feature at high latitudes in a recent survey based on Cluster observations (Fuselier et al, 2018). This means that there are two possibilities of reconnection associated with the formation of HiLDA: lobe reconnection or non-lobe reconnection.…”

Section: Accepted Articlesupporting

confidence: 93%

“…The reconnection poleward of the cusp separates the TPA and the HiLDA into two different regions with the former on closed field lines and latter on open field lines. Moreover, reconnection with closed magnetic field lines poleward of the cusp is sometime called non‐lobe reconnection, which has been suggested to be a common feature at high latitudes in a recent survey based on Cluster observations (Fuselier et al., 2018). This means that there are two possibilities of reconnection associated with the formation of HiLDA: lobe reconnection or non‐lobe reconnection.…”

Section: Discussionmentioning

confidence: 99%

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DMSP Observations of High‐Latitude Dayside Aurora (HiLDA)

et al. 2021

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Section: Accepted Articlesupporting

confidence: 93%

Section: Discussionmentioning

confidence: 99%

DMSP Observations of High‐Latitude Dayside Aurora (HiLDA)

et al. 2021

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“…Magnetopause reconnection enabled by foreshock turbulence presents a new possible scenario of dayside reconnection when the IMF clock angle (between the IMF B yz and z GSM ) is ~0, as in the simulated case. The known scenarios are: (1) reconnection of IMF with open cusp field lines (lobe reconnection), and (2) reconnection of IMF with closed field lines that thread through the nightside of the magnetosphere (non-lobe reconnection), as illustrated inFuselier et al [2018]. Foreshock turbulence makes possible for local bursty reconnection to occur near the subsolar magnetopause by creating large shear angles between the magnetosheath and the magnetosphere fields.…”

mentioning

confidence: 99%

Magnetopause Reconnection and Indents Induced by Foreshock Turbulence

Chen

Omelchenko

et al. 2021

Geophysical Research Letters

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Magnetopause reconnection plays a critical role in controlling energy input from the solar wind to the magnetosphere. The possibility that magnetic fluctuations generated in the foreshock may lead to magnetopause reconnection has been considered based on observations indicating that magnetosheath fields are not a simple compression of the interplanetary magnetic field (IMF) (Russell et al., 1997;Zhang et al., 1997). On account of the fact that the statistical magnetopause locations for cone angles (between the IMF and the Sun-Earth line) greater and less than 45° do not differ appreciably, the study by Zhang et al. (1997) concludes that the raised possibility is not confirmed. Recent measurements from the Magnetospheric Multiscale mission show Earth-radius-scale foreshock magnetic and density fluctuations approximately one order of magnitude larger than the respective upstream values under quasi-radial IMF (cone angles <30°) conditions (Chen et al., 2021). These intense fluctuations often contain strong B z (in Geocentric Solar magnetic (GSM) coordinates) and B y components. If these fluctuations can reach the magnetopause, they can create conditions conducive to reconnection. In this paper, based on global hybrid simulation results, we predict that foreshock fluctuations in the form of strong B z and density fluctuations can reach the magnetopause and lead to reconnection as well as Earth-sized indents.To single out the effects of foreshock fluctuations, we design our simulation to have a quasi-radial IMF with a weak northward (B z > 0) and zero dawn-dusk (B y = 0) components. When the IMF is quasi-radial, foreshock waves excited due to reflected ions interacting with the incoming solar wind are the strongest, permeate the largest volume of the subsolar region, and can most strongly influence the inner magnetosphere (e.g., Russell et al.,1983; Takahashi et al., 2021, and references therein). In the aspect of reconnection, extensive statistical studies show that magnetopause reconnection occurs for shear angles (angle between the magnetosheath and magnetosphere magnetic fields across the magnetopause) as low as ∼30° but not lower than that (e.g.,

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“…These phenomena have not been observed previously for electrons, but similar phenomena have been studied for ions. The decrease of the cutoff velocity of the curved D shape ion distribution caused by the E×B drift has been observed in PIC simulation (Broll et al, 2017; ignoring the effect of wave-particle interactions) and cluster observation (Fuselier et al, 2018). Therefore, both of these two dispersions are caused by the E×B drift; however, the time for E×B drift is different.…”

Section: Discussionmentioning

confidence: 88%

Electron Dispersion and Parallel Electron Beam Observed Near the Separatrix

et al. 2019

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The separatrix region is the region between the separatrix and the reconnection jet. Due to the E×B drift and velocity filter effect in which high‐energy particles with high parallel speed can be seen prior to low‐energy particles along the field line, electrons are separated from ions. The electron dynamics in this region is of interest; however it has not been studied in detail, because of the insufficient resolution of plasma data. We present a slow separatrix crossing event observed by Magnetospheric Multiscale (MMS) satellite constellation on 1 January 2016, from the magnetosheath side with high‐resolution burst mode data. The electron edge and ion edge are clearly distinguished in the separatrix region. Two types of electron dispersion, one with a short duration (~0.3 s) and the other with a longer duration (~13 s) were detected between the electron and ion edges. The rapid dispersion (with small time scale) is mainly in the parallel direction, which might originate from a thin layer with non‐frozen‐in electrons close to the separatrix. The gradual (long time scale) dispersion is seen from parallel to perpendicular directions, which comes from the E×B drift of a curved D‐shape distribution of electrons. The width of the electron diffusion region on the magnetosheath side is estimated based on MMS observation. The observation also reveals an unexpected parallel electron beam outside of the electron edge. Wave‐particle interaction or parallel potential in the inflow region may be responsible for the generation of this electron population.

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Nonlobe Reconnection at the Earth's Magnetopause for Northward IMF

Cited by 11 publications

References 34 publications

DMSP Observations of High‐Latitude Dayside Aurora (HiLDA)

DMSP Observations of High‐Latitude Dayside Aurora (HiLDA)

Magnetopause Reconnection and Indents Induced by Foreshock Turbulence

Electron Dispersion and Parallel Electron Beam Observed Near the Separatrix

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