Modeling the magnetosphere for northward interplanetary magnetic field: Effects of electrical resistivity

Raeder, J.

doi:10.1029/1999ja900159

Cited by 65 publications

(74 citation statements)

References 37 publications

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“…In a recent article Raeder [1999] presented a series of MHD simulations using a resistive MHD model to describe the interaction of the terrestrial magnetosphere with the solar wind for due northward interplanetary magnetic field (IMF) conditions. Depending on the initial conditions, the simulated magnetotail remained open for at least 6 hours after the IMF turned from south to north, or remained closed at all times when the simulation started with northward IMF.…”

Section: Introductionmentioning

confidence: 99%

Comment on “Modeling the magnetosphere for northward interplanetary magnetic field: Effects of electrical resistivity” by Joachim Raeder

Gombosi¹,

Powell²,

Leer³

2000

J. Geophys. Res.

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Section: Introductionmentioning

confidence: 99%

Comment on “Modeling the magnetosphere for northward interplanetary magnetic field: Effects of electrical resistivity” by Joachim Raeder

Gombosi¹,

Powell²,

Leer³

2000

J. Geophys. Res.

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“…Figure 5 shows the time evolution of the magnetospheric configuration after northward turning of the IMF at t = 0, when starting with a steady state magnetosphere under southward IMF. As a counterargument against numerical diffusion in the BATS-R-US code being responsible for the closed magnetosphere Gombosi et al (2000) point out the high resistivity case of Raeder (1999) leads to a highly diffused bow shock, whereas in the Gombosi et al /Song et al simulations the bow shock is very well resolved. In his reply Raeder (2000) stresses first that none of the codes listed by Gombosi et al (2000), which result in a closed magnetosphere, really quantify the diffusivity in their codes.…”

Section: Global Simulations: Northward Imfmentioning

confidence: 99%

“…Models which lead rapidly to a short and closed magnetosphere under northward IMF may simply exhibit higher reconnection rates at the lobe reconnection sites. However, recently Raeder (1999) has suggested that numerical diffusion may be another factor leading to rapid closing of the magnetosphere under northward IMF. To prove this Raeder (1999) has run his code with different values of the (spatially constant) resistivity.…”

Section: Global Simulations: Northward Imfmentioning

confidence: 99%

“…However, recently Raeder (1999) has suggested that numerical diffusion may be another factor leading to rapid closing of the magnetosphere under northward IMF. To prove this Raeder (1999) has run his code with different values of the (spatially constant) resistivity. By increasing the resistivity he eventually obtains a magnetosphere without open lobe field lines, and the tail length decreases with increasing resistivity, reaching a tail length as short as 50 R E in the highest resistivity case.…”

Section: Global Simulations: Northward Imfmentioning

confidence: 99%

“…Similar low overheads have stretched Cartesian grids, where the highest resolution is assumed to be near Earth and the resolution diminishes in the tailward direction. Such a non-uniform grid with near-Earth resolution of 0.5 R E is used by Raeder (1999). Adaptive grid schemes partition space into regions according to the gradients in solutions of physical quantities: in a region where large gradients exist, the resolution will be refined.…”

Section: Numerical Gridsmentioning

confidence: 99%

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Space Storms and Space Weather Hazards

Daglis¹

2001

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Subject Terms Report Classification unclassified Classification of this page unclassified Classification of Abstract unclassified Limitation of Abstract UU Number of Pages 486REPORT DOCUMENTATION PAGE Public reporting burden for this collection of information is estimated to average 1 hour per response, including the time for reviewing instructions, searching existing data sources, gathering and maintaining the data needed, and completing and reviewing the collection of information. Send comments regarding this burden estimate or any other aspect of this collection of information, including suggestions for reducing this burden to Washington Headquarters Services, Directorate for Information Operations and Reports, 1215 Jefferson Davis Highway, Suite 1204, Arlington, VA 22202-4302, and to the Office of Management and Budget, -to review recent spacecraft measurements that have provided new insight into the dynamics and effects of space storms; -to review space weather hazards associated with space storms and pertinent to the operation of technological systems in space and on ground;-to discuss and assess methods of space weather forecasting, as well as national and international initiatives towards an efficient development of space climatology.Space weather, the invisible but nevertheless effective result of solar activity and solar-terrestrial coupling, has affected the operations of communication systems since the appearance of telegraph in the 19th century, though as an unknown trouble factor. Nowadays, the effects of space weather affect in various ways all communication modes, from cable to wireless to space-based systems. Moreover, space weather hazards include malfunction or even permanent damage of power distribution grids and of telecommunication, navigation and surveillance satellites, disturbances of over-the-horizon (OTH) radar, HF, VHF and UHF communications, surveying and navigation systems that use Global Positioning System (GPS) satellites, surveillance (optical and radar), and satellite tracking. Space weather influences on the Earth's weather and climate is still a developing topic. Little is known concerning the biological effects of space weather, especially regarding astronauts.This Institute could not be timelier. Space Weather, which has been defined as "conditions on the sun and in the solar wind, magnetosphere, ionosphere, and thermosphere that can influence the performance and reliability of space-and ground-based technological systems and can endanger human life", encompasses a broad range of phenomena impacting both space science and technology. The effects of Space Weather, while present throughout the solar cycle, gain particular prominence around the peak of the 11-year sunspot activity; the maximum of cycle 23 occurred in summer 2000.The fact that this ASI on Space Weather was held in Europe is particularly appropriate. European countries host a considerable repository of knowledge and world-class facilities in this field. Nevertheless, while Space Weather activities in c...

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Collisionless resistivity in a bifurcated current sheet

Andriyas

Spencer

2014

JGR Space Physics

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The collisionless resistivity due to charged particle chaos in spatially inhomogeneous magnetic fields is calculated for two frequently observed magnetotail current sheets, the X line, and a bifurcated current sheet (BCS) over varying strengths of cross-tail electric field. The calculation is done for two charged species, protons and O + ions, found in the magnetotail specially during active times. Chaotic behavior of the particles is studied for the chaos parameter ≈ 1 defined by Buchner and Zelenyi (1989) as the square root of minimum radius of curvature to the maximum particle gyroradius. The surface of section plot and maximal Lyapunov exponents are analyzed to compare the particle behavior in the two magnetic field topologies. It is found that the particle behavior in a BCS is chaotic around the two humps located at ±z 0 and that the configuration is more chaotic than the X line (maximum Lyapunov exponent for X line is around 0.25 compared to 0.34 for BCS). The collisionless resistivity is calculated using the technique developed by Numata and Yoshida (2003). The method relies on a phenomenological equivalence between the particle loss rate from the chaos region and rate of change of momentum in the chaos region under steady state conditions. Rapid decay of the particles from the chaos region is modeled with exponential fits, and it is found that a double exponent is needed for O + ions in an X line and for both species in the BCS. The resistivity thus calculated is found to be 9-10 orders of magnitude higher than the Spitzer resistivity.

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Modeling the magnetosphere for northward interplanetary magnetic field: Effects of electrical resistivity

Cited by 65 publications

References 37 publications

Comment on “Modeling the magnetosphere for northward interplanetary magnetic field: Effects of electrical resistivity” by Joachim Raeder

Comment on “Modeling the magnetosphere for northward interplanetary magnetic field: Effects of electrical resistivity” by Joachim Raeder

Space Storms and Space Weather Hazards

Collisionless resistivity in a bifurcated current sheet

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