Statistical Comparison of Various Dayside Magnetopause Reconnection X‐Line Prediction Models

Qudsi, Ramiz A.; Walsh, Brian M.; Broll, Jeff; Atz, Emil; Haaland, Stein

doi:10.1029/2023ja031644

Cited by 3 publications

(3 citation statements)

References 41 publications

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“… 2016 ; Qudsi et al. 2023 ). Although the magnetic field orientation and plasma pressure on the magnetospheric side of the magnetopause are relatively constant (Tsyganenko and Sitnov 2007 ), the parameters in the magnetosheath vary significantly on time scales of minutes based on the driving solar wind (Dimmock et al.…”

Section: Science Objectives and Backgroundmentioning

confidence: 99%

The Lunar Environment Heliophysics X-ray Imager (LEXI) Mission

Walsh,

Kuntz,

Busk

et al. 2024

Space Sci Rev

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The Lunar Environment heliospheric X-ray Imager (LEXI) is a wide field-of-view soft X-ray telescope developed to study solar wind-magnetosphere coupling. LEXI is part of the Blue Ghost 1 mission comprised of 10 payloads to be deployed on the lunar surface. LEXI monitors the dayside magnetopause position and shape as a function of time by observing soft X-rays (0.1–2 keV) emitted from solar wind charge-exchange between exospheric neutrals and high charge-state solar wind plasma in the dayside magnetosheath. Measurements of the shape and position of the magnetopause are used to test temporal models of meso- and macro-scale magnetic reconnection. To image the boundary, LEXI employs lobster-eye optics to focus X-rays to a microchannel plate detector with a 9.1$^{\circ }\times 9.1^{\circ }$ × ∘ 9.1 ∘ field of view.

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Section: Science Objectives and Backgroundmentioning

confidence: 99%

The Lunar Environment Heliophysics X-ray Imager (LEXI) Mission

Walsh,

Kuntz,

Busk

et al. 2024

Space Sci Rev

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“…Note also that bisection is used in the Moore et al. model to find the location of the X line along the global magnetopause (Moore et al., 2002; Qudsi et al., 2022).…”

Section: Introductionmentioning

confidence: 99%

“…The orientation based on bisection was similar to that of several other theoretical predictions (Liu et al, 2018), but significantly different from the M direction as defined above. Note also that bisection is used in the Moore et al model to find the location of the X line along the global magnetopause (Moore et al, 2002;Qudsi et al, 2022).…”

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confidence: 99%

Determining the Orientation of a Magnetic Reconnection X Line and Implications for a 2D Coordinate System

Denton,

Liu,

Agudelo Rueda

et al. 2024

JGR Space Physics

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An LMN coordinate system for magnetic reconnection events is sometimes determined by defining N as the direction of the gradient across the current sheet and L as the direction of maximum variance of the magnetic field. The third direction, M, is often assumed to be the direction of zero gradient, and thus the orientation of the X line. But when there is a guide field, the X line direction may have a significant component in the L direction defined in this way. For a 2D description, a coordinate system describing such an event would preferably be defined using a different coordinate direction M′ oriented along the X line. Here we use a 3D particle‐in‐cell simulation to show that the X line is oriented approximately along the direction bisecting the asymptotic magnetic field directions on the two sides of the current sheet. We describe two possible ways to determine the orientation of the X line from spacecraft data, one using the minimum gradient direction from Minimum Directional Derivative analysis at distances of the order of the current sheet thickness from the X line, and another using the bisection direction based on the asymptotic magnetic fields outside the current sheet. We discuss conditions for validity of these estimates, and we illustrate these conditions using several Magnetospheric Multiscale (MMS) events. We also show that intersection of a flux rope due to secondary reconnection with the primary X line can destroy invariance along the X line and negate the validity of a two‐dimensional description.

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Magnetic fields and electric currents around the dayside magnetopause as inferred from data-constrained modeling

Tsyganenko,

Semenov,

Erkaev

et al. 2024

Front. Astron. Space Sci.

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Based on a new mathematical framework and large multi-year multi-mission data sets, we reconstruct electric currents and magnetic fields around the dayside magnetopause and their dependence on the incoming solar wind, IMF, and geodipole tilt. The model architecture builds on previously developed mathematical frameworks and includes two separate blocks: for the magnetosheath and for the adjacent outer magnetosphere. Accordingly, the model is developed in two stages: 1) reconstruction of a best-fit magnetopause and underlying dayside magnetosphere, based on a simple shielded configuration, and 2) derivation of the magnetosheath magnetic field, represented by a sum of toroidal and poloidal terms, each expanded into spherical harmonic series of angular coordinates and powers of normal distance from the boundary. The spacecraft database covers the period from 1995 through 2022 and is composed of data from Geotail, Cluster, Themis, and MMS, with the total number of 1-min averages about 3 M. The modeling reveals orderly patterns of the IMF draping around the magnetosphere and of the magnetopause currents, controlled by the IMF orientation, solar wind pressure, and the Earth’s dipole tilt. The obtained results are discussed in terms of the magnetosheath flux pile-up and the dayside magnetosphere erosion during periods of northward or southward IMF, respectively.

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Statistical Comparison of Various Dayside Magnetopause Reconnection X‐Line Prediction Models

Cited by 3 publications

References 41 publications

The Lunar Environment Heliophysics X-ray Imager (LEXI) Mission

The Lunar Environment Heliophysics X-ray Imager (LEXI) Mission

Determining the Orientation of a Magnetic Reconnection X Line and Implications for a 2D Coordinate System

Magnetic fields and electric currents around the dayside magnetopause as inferred from data-constrained modeling

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