A model of the steady state magnetic field in the magnetosheath

Kobel, E.; Flückiger, E. O.

doi:10.1029/94ja01778

Cited by 123 publications

(224 citation statements)

References 11 publications

(7 reference statements)

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“…In this study, we have modified the analysis by considering actual dipole tilt angles calculated for the time intervals of interest. In addition (as mentioned above), the draping of the magnetosheath field about the magnetopause is also more realistic (utilizing the Kobel and Flückiger [1994] …”

Section: Instrumentation and Methodologymentioning

confidence: 99%

“…For the analytic model of the external (magnetosheath) magnetic field, the Cooling et al [2001] magnetopause is used as the inner boundary. The Cooling et al [2001] magnetic field model is a restricted version of the more general Kobel and Flückiger [1994] model (which is an analytic representation of the magnetic field throughout the magnetosheath). This boundary is described by a paraboloid with the focus located on the Sun-Earth line, exactly halfway between the Earth and the magnetopause subsolar location.…”

Section: Instrumentation and Methodologymentioning

confidence: 99%

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Probing the boundary between antiparallel and component reconnection during southward interplanetary magnetic field conditions

et al. 2007

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[1] One of the major outstanding questions about magnetic reconnection is where reconnection will occur at the Earth's magnetopause for specific conditions of the solar wind and the interplanetary magnetic field (IMF). There are two scenarios discussed in the literature: (1) antiparallel reconnection, which occurs where the magnetospheric magnetic field and the IMF are antiparallel (shear angle of approximately 180°) and (2) component reconnection, where shear angles between the magnetospheric field and the IMF as low as 50°have been reported. The distinction between the two reconnection scenarios is important for the energy and momentum transfer from the solar wind to the magnetosphere. Here we report on a method using three-dimensional plasma observations from the Toroidal Imaging Mass-Angle Spectrograph instrument on the Polar spacecraft as it passes through the northern magnetospheric cusp to calculate the distance to the reconnection line and subsequently trace the distance along model magnetic field lines back to the magnetopause. Results from 130 events reveal that in general, magnetic reconnection occurs along an extended line across the dayside magnetopause (i.e., consistent with the component reconnection scenario). During strong sunward or antisunward IMF conditions (B X ), however, the reconnection location resembles the antiparallel reconnection model at high latitudes and does not cross the dayside magnetopause as a single tilted reconnection line. These results show that either reconnection scenario can occur at the magnetopause, depending on the specific IMF conditions. Citation: Trattner, K. J., J. S. Mulcock, S. M. Petrinec, and S. A. Fuselier (2007), Probing the boundary between antiparallel and component reconnection during southward interplanetary magnetic field conditions,

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Section: Instrumentation and Methodologymentioning

confidence: 99%

Section: Instrumentation and Methodologymentioning

confidence: 99%

Probing the boundary between antiparallel and component reconnection during southward interplanetary magnetic field conditions

et al. 2007

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“…The Cooling model calculates the magnetosheath magnetic field (B ms ) from a model developed by Kobel and Flückiger (1994). The Kobel and Flückiger (1994) model takes three inputs: the stand-off distances of the bow shock and magnetopause (R bs and R mp ) and the IMF.…”

Section: The Cooling Modelmentioning

confidence: 99%

“…The Kobel and Flückiger (1994) model takes three inputs: the stand-off distances of the bow shock and magnetopause (R bs and R mp ) and the IMF. The magnetopause is modelled as a paraboloid.…”

Section: The Cooling Modelmentioning

confidence: 99%

Motion of flux transfer events: a test of the Cooling model

et al. 2007

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Abstract. The simple model of reconnected field line motion developed by Cooling et al. (2001) has been used in several recent case studies to explain the motion of flux transfer events across the magnetopause. We examine 213 FTEs observed by all four Cluster spacecraft under a variety of IMF conditions between November 2002 and June 2003, when the spacecraft tetrahedron separation was ∼5000 km. Observed velocities were calculated from multi-spacecraft timing analysis, and compared with the velocities predicted by the Cooling model in order to check the validity of the model. After excluding three categories of FTEs (events with poorly defined velocities, a significant velocity component out of the magnetopause surface, or a scale size of less than 5000 km), we were left with a sample of 118 events. 78% of these events were consistent in both direction of motion and speed with one of the two model de Hoffmann-Teller (dHT) velocities calculated from the Cooling model (to within 30 • and a factor of two in the speed). We also examined the plasma signatures of several magnetosheath FTEs; the electron signatures confirm the hemisphere of connection indicated by the model in most cases. This indicates that although the model is a simple one, it is a useful tool for identifying the source regions of FTEs.

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“…Figure 6.6, on the other hand, shows significant Z-component in the field which may be attributed to the nonaxisymmetric magnetosheath as advocated by Erkaev et al (1996) and this is further interpreted in §6.4. Kobel and Flückiger [1994] developed an analytical model (herein referred to as KF94) to characterize the magnetic field in the magnetosheath which has been used extensively in Earth studies [e.g. Longmore et al, 2006;Cooling et al, 2001;Petrinec, 2012] and/or profiles showing how the magnetic field evolves as a consequence of nonaxisymmetry along the subsolar line in the magnetosheasth [Erkaev et al, 1996;Farrugia et al, 1998].…”

Section: Mhd Simulationsmentioning

confidence: 99%

The Near-Saturn Magnetic Field Environment

Sulaiman

2017

Springer Theses

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Shock waves exist throughout the universe and are fundamental to understanding the nature of collisionless plasmas. The complex coupling between charged particles and electromagnetic fields in plasmas give rise to a whole host of mechanisms for dissipation and heating across shock waves, particularly at high Mach numbers. While ongoing studies have investigated these process extensively both theoretically and via simulations, their observations remain few and far between. This thesis presents a study of very high Mach number shocks in a parameter space that has been poorly explored and identifies reformation using in situ magnetic field observations from the This non-axisymmetry is revealed to have an impact in the rotation of the magnetic field and is significant enough to influence the magnetic shear at the magnetopause.

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A model of the steady state magnetic field in the magnetosheath

Cited by 123 publications

References 11 publications

Probing the boundary between antiparallel and component reconnection during southward interplanetary magnetic field conditions

Probing the boundary between antiparallel and component reconnection during southward interplanetary magnetic field conditions

Motion of flux transfer events: a test of the Cooling model

The Near-Saturn Magnetic Field Environment

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