<i>Solar Magnetohydrodynamics</i>

Priest, E. R.; Low, B. C.

doi:10.1063/1.2915760

Cited by 174 publications

(277 citation statements)

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“…where r is heliocentric distance, U is the bulk solar wind speed, n {e,p} is the electron (proton) number density, Q {e,p} represents turbulent heating per unit mass, q e is the electron heat flux vector (proton heat flux vector has been neglected), and k B is Boltzmann's constant. The T e À T p terms in equations (1) -(2) model Coulomb collisions taking place over a timescale t [e.g., Priest, 1982].…”

Section: Introductionmentioning

confidence: 99%

Electron and proton heating by solar wind turbulence

et al. 2009

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[1] Previous formulations of heating and transport associated with strong magnetohydrodynamic (MHD) turbulence are generalized to incorporate separate internal energy equations for electrons and protons. Electron heat conduction is included. Energy is supplied by turbulent heating that affects both electrons and protons and is exchanged between them via collisions. Comparison to available Ulysses data shows that a reasonable accounting for the data is provided when (1) the energy exchange timescale is very long and (2) the deposition of heat due to turbulence is divided, with 60% going to proton heating and 40% into electron heating. Heat conduction, determined here by an empirical fit, plays a major role in describing the electron data.

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Section: Introductionmentioning

confidence: 99%

Electron and proton heating by solar wind turbulence

et al. 2009

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“…and Mach numbers M A are low enough, then a fast ''switchon'' shock can occur. In this regime, the magnetic field downstream of the shock has components parallel to the shock surface, whereas upstream B IMF is parallel to n. From the jump conditions of a MHD shock, the criteria for the switch-on solution can be written as [e.g., Priest, 1982] b < 2=g ð4Þ…”

Section: Introductionmentioning

confidence: 99%

MHD simulations of Earth's bow shock: Interplanetary magnetic field orientation effects on shape and position

et al. 2004

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[1] The location and geometry of Earth's bow shock vary considerably with the solar wind conditions. More specifically, Earth's bow shock is formed by the steepening of fast mode waves, whose speed v ms depends upon the angle q bn between the local shock normal n and the magnetic field vector B IMF , as well as the Alfvén and sound speeds (v A and c S ). Since v ms is a minimum for q bn = 0°and low Alfvén Mach number M A , and maximum for q bn = 90°and high M A , this implies that as q IMF (the angle between B IMF and v sw ) varies, the magnitude of v ms should vary also across the shock, leading to changes in shape. This paper presents 3-D MHD simulation data which illustrate the changes in shock location and geometry in response to changes in q IMF and M A , for 1.4 M A 9.7 and 0° q IMF 90°. Specifically, for oblique IMF the shock's geometry is shown to become skewed in planes containing B IMF (e.g., the x À z plane). This is also emphasized in the terminator plane data, where the shock is best represented by ellipses, with centers translated along the z axis. For the q IMF = 90°simulations the shock is symmetric about the x axis in both the x À y and x À z planes. Simulations for fieldaligned flow (q IMF = 0°) show a dimpling of the nose of the shock as M A ! 1. The simulations also illustrate the general movement of the shock in response to changes in M A ; high M A shocks are found closer to Earth than low M A shocks. Farris et al. 's [1991] magnetopause model is used in the simulations, and we discuss the limitations of this, as well as the expected results using a self-consistent model.

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“…[8] The global-scale dynamics in the interplanetary solar wind can be theoretically modeled by the following MHD equations [Priest, 1982;Hughes and Brighton, 1967] in SI units; this procedure is identical with the previous study [Wu et al, 2005c, hereinafter referred to as Paper 1].…”

Section: Magnetohydrodynamics Equationsmentioning

confidence: 99%

Effects of the interaction and evolution of interplanetary shocks on “background” solar wind speeds

Feng

et al. 2006

J. Geophys. Res.

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[1] Solar wind speed plays an important role in the study of space weather prediction. Some workers have used it for measuring the arrival time of solar disturbances at 1 AU. The purpose of this work is to extend our previous study (Wu et al., 2005c) of some Halloween 2003 events by presenting additional physical effects of multiple shock interactions on the solar wind profile during a complex compound event. In order to achieve this goal, we track a group of specific solar events' plasma and magnetic field output as they propagate into interplanetary space. A one-dimensional, time-dependent adaptive grid MHD code is used to study the evolution and interaction of shocks from Sun through the heliosphere. The MHD simulation results demonstrate that the solar wind speed might increase about %25% after two shocks collide with each other. This kind of interaction can affect the accuracy of the identification of the solar source that causes the interplanetary event (e.g., magnetic cloud, coronal mass ejection, interplanetary shock, or some other interplanetary discontinuity.) In this study we further simulate part of the famous Halloween 2003 events that contain at least four major solar events (flares) during 28 October to 1 November 2003. These major events, simulated by pressure pulses, generated shocks that matched well with ACE (Advanced Composition Explorer) observations as reported by Wu et al. (2005c) in our previous study. The present work presents new details concerning the interplay (such as sunward and antisunward traveling compression and rarefaction waves) between fast forward and fast reverse interplanetary shocks.

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Solar Magnetohydrodynamics

Cited by 174 publications

References 0 publications

Electron and proton heating by solar wind turbulence

Electron and proton heating by solar wind turbulence

MHD simulations of Earth's bow shock: Interplanetary magnetic field orientation effects on shape and position

Effects of the interaction and evolution of interplanetary shocks on “background” solar wind speeds

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