Interaction between the solar plasma wind and the geomagnetic cavity

Lees, Lester

doi:10.2514/3.2622

Cited by 133 publications

(55 citation statements)

References 23 publications

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“…Although this formula was obtained from simulations of earthÕs magnetosheath, we use it also to specify the field strength in the magnetosheath of the ICME, for several such algorithms we have considered (e.g., Lees, 1964), none has more physical justification. To apply Eq.…”

Section: Interpretation and Set Upmentioning

confidence: 99%

Dst of the Carrington storm of 1859

Siscoe

Crooker

Clauer

2006

Advances in Space Research

150

171

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Section: Interpretation and Set Upmentioning

confidence: 99%

Dst of the Carrington storm of 1859

Siscoe

Crooker

Clauer

2006

Advances in Space Research

150

171

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“…(One must handle this anal ogy with care, however, since draping depends on the dimensionality of the problem: e.g., draping about a straight cylinder is a two-dimensional problem while draping around the magnetosphere is inherently threedimensional.) Theoretical studies of MHD flow past the magnetosphere predict the occasional presence of a "magnetic barrier" (aliter: "depletion layer") adjacent to the sunward side of the magnetopause [Midgley and Davis, 1963;Lees, 1964;Zwan and Wolf, 1976;Erkaev, 1988]. Spacecraft passes through the low-latitude, dayside magnetosheath next to the magnetopause routinely reveal the presence of a depletion layer when the local magnetic shear across the magnetopause, angle tp, is small (< 30°) [Phan et al, 1994, and references therein], though a depletion layer should also be present irrespec tive of magnetic shear when the solar wind Alfven Mach number, MA, is low [Farrugia et al, 1995b[Farrugia et al, , 1996.…”

Section: Magnetic Field Line Draping Around and Magnetic Barriers Ahmentioning

confidence: 99%

Magnetic clouds and the quiet-storm effect at Earth

1997

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In this review, we discuss first magnetic clouds in the context of other interplanetary causes of geomagnetic storms. We then describe work on the global field line topology of magnetic clouds, focussing on information gained by the use of energetic particles. We then give a summary of theoretical and simulation work on the dynamics of magnetic clouds. In one approach, based on self-similar evolution of radially expanding magnetic flux ropes, the role of electrons is central. A section on the boundaries of magnetic clouds is followed by one on magnetic field line draping around these ejecta, including the formation of a magnetic barrier. In the aspect of the study dealing with the geomagnetic response to magnetic clouds, we discuss effects on the dayside magnetosheath; ionosphere; and nightside magnetosphere at geostationary orbit and beyond, utilizing primarily observations made during Earth's encounter with a magnetic cloud on January, 13 -14, 1988. A case study is mentioned where solar energetic particles, injected into a magnetic cloud and then guided along its helical field lines, entered the magnetosphere through interconnection of the cloud's field lines with those of Earth. Simulation work on the geomagnetic response to magnetic clouds is briefly reviewed. We finally consider studies specifically correlating magnetic clouds, in isolation or as part of compound streams, with geomagnetic storm activity. Throughout, we indicate areas where further work is needed.

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“…Boundary layers are formed also upstream of the Earth's magnetopause (Zwan & Wolf 1976), where they are called the plasma depletion layers (PDLs). Following Lees (1964) and Alksne (1967), it was shown that a PDL on the surface of the magnetosphere creates magnetic stress that affects the plasma flow. The width of such depletion layer was estimated to be about 700-1300 km for the Earth magnetosphere at 10 R E for the SW Alfvén number M A = 8 and rapidly decreasing as M A increases.…”

Section: Bow Wave and Heliospheric Boundary Layermentioning

confidence: 99%

Three-dimensional Features of the Outer Heliosphere Due to Coupling between the Interstellar and Heliospheric Magnetic Field. V. The Bow Wave, Heliospheric Boundary Layer, Instabilities, and Magnetic Reconnection

Pogorelov

Heerikhuisen

Roytershteyn

et al. 2017

ApJ

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The heliosphere is formed due to interaction between the solar wind (SW) and local interstellar medium (LISM). The shape and position of the heliospheric boundary, the heliopause, in space depend on the parameters of interacting plasma flows. The interplay between the asymmetrizing effect of the interstellar magnetic field and charge exchange between ions and neutral atoms plays an important role in the SW-LISM interaction. By performing three-dimensional, MHD plasma / kinetic neutral atom simulations, we determine the width of the outer heliosheath -the LISM plasma region affected by the presence of the heliosphere -and analyze quantitatively the distributions in front of the heliopause.It is shown that charge exchange modifies the LISM plasma to such extent that the contribution of a shock transition to the total variation of plasma parameters becomes small even if the LISM velocity exceeds the fast magnetosonic speed in the unperturbed medium. By performing adaptive mesh refinement simulations, we show that a distinct boundary layer of decreased plasma density and enhanced magnetic field should be observed on the interstellar side of the heliopause. We show that this behavior is in agreement with the plasma oscillations of increasing frequency observed by the plasma wave instrument onboard Voyager 1. We also demonstrate that Voyager observations in the inner heliosheath between the heliospheric termination shock and the heliopause are consistent with dissipation of the heliospheric magnetic field. The choice of LISM parameters in this analysis is based on the simulations that fit observations of energetic neutral atoms performed by IBEX.

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Interaction between the solar plasma wind and the geomagnetic cavity

Cited by 133 publications

References 23 publications

Dst of the Carrington storm of 1859

Dst of the Carrington storm of 1859

Magnetic clouds and the quiet-storm effect at Earth

Three-dimensional Features of the Outer Heliosphere Due to Coupling between the Interstellar and Heliospheric Magnetic Field. V. The Bow Wave, Heliospheric Boundary Layer, Instabilities, and Magnetic Reconnection

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