In-Situ Observations of Reconnection in Space

Paschmann, G.; Øieroset, M.; Phan, T. D.

doi:10.1007/s11214-012-9957-2

Cited by 176 publications

(166 citation statements)

References 161 publications

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“…Magnetic reconnection is in itself one of the most important phenomena that can occur in plasmas, and in the context of the magnetosphere is an important topic of study in its own right (for recent reviews see e.g., Paschmann et al 2013). It enables the formation of open field lines, connected to the Earth in one direction and into the solar wind in the other direction.…”

Section: Magnetic Reconnectionmentioning

confidence: 99%

What Controls the Structure and Dynamics of Earth’s Magnetosphere?

et al. 2014

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Unlike most cosmic plasma structures, planetary magnetospheres can be extensively studied in situ. In particular, studies of the Earth's magnetosphere over the past few decades have resulted in a relatively good experimental understanding of both its basic structural properties and its response to changes in the impinging solar wind. In this article we provide a broad overview, designed for researchers unfamiliar with magnetospheric physics, of the main processes and parameters that control the structure and dynamics of planetary magnetospheres, especially the Earth's. In particular, we concentrate on the structure and dynamics of three important regions: the bow shock, the magnetopause and the magnetotail. In the final part of this review we describe the current status of global magnetospheric modelling, which is crucial to placing in situ observations in the proper context and providing a better understanding of magnetospheric structure and dynamics under all possible input conditions. Although the parameter regime experienced in the solar system is limited, the plasma physics that is learned by studying planetary magnetospheres can, in principle, be translated to more general studies of cosmic plasma structures. Conversely, studies of cosmic plasma under a wide range of conditions should be used to understand Earth's

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Section: Magnetic Reconnectionmentioning

confidence: 99%

What Controls the Structure and Dynamics of Earth’s Magnetosphere?

et al. 2014

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“…Further dissipationless cascading toward electron gyro ρ e = v e /ω ce ≡ λ e / √ β e and inertial scales λ e = c/ω e spans the length interval λ i ℓ λ e , roughly ∼ 2 orders of magnitude in a proton-electron plasma. When the cascade approaches its smallscale end ℓ λ e the narrow filamentary current eddies enter the range of collisionless reconnection [for reviews of reconnection observations and theory see 13,14] 19) due to thermal electron meandering in the current layer resulting in large electron-shear viscosity. This was simulationally confirmed [20] yielding the lower-hybrid frequency ω lh [21] as robust absolute upper limit on the dissipation rate for the magnetic energy that is fed into formation of small-scale currents [cf., 22, for astrophysical application].…”

Section: Introductionmentioning

confidence: 99%

Ideal MHD turbulence: the inertial range spectrum with collisionless dissipation

2015

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Citation:Treumann RA, Baumjohann W and Narita Y (2015) The inertial range spectrum of ideal (collisionless/dissipationless) MHD turbulence is analyzed in view of the transition from the large-scale Iroshnikov-Kraichnan-like (IK) to the meso-scale Kolmogorov (K) range under the assumption that the ultimate dissipation which terminates the Kolmogorov range is provided by collisionless reconnection in thin turbulence-generated current sheets. Kolmogorov's dissipation scale is identified with the electron inertial scale, as suggested by collisionless particle-in-cell simulations of reconnection. Transition between the IK-and K-ranges occurs at the ion inertial length allowing determination of the IK-coefficient. With the electron inertial scale the K-dissipation scale, stationarity of the spectrum implies a relation between the energy injection and dissipation rates. Application to solar wind is critically discussed.

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“…Indeed, in recent years, taking advantage of a mass of high quality in situ observations and numerical simulations, appreciable steps forward have been done toward the comprehension of reconnection (see the recent reviews from Priest & Forbes 2000;Paschmann et al 2013;Treumann & Baumjohann 2013). It has been ascertained that reconnection is collisionless (see e.g., Øieroset et al 2001, 2002) and that for reconnection to initiate, the current sheet thickness has to be smaller than the ion inertial length (see, e.g., Cassak et al 2006).…”

Section: Introductionmentioning

confidence: 99%

Statistical and Scaling Features of Fluctuations in the Dissipation Range During a Reconnection Event

Consolini

Grandioso

Yordanova

et al. 2015

ApJ

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Reconnection events in space plasmas are accompanied by the occurrence of large-amplitude turbulent fluctuations of the magnetic and electric field, covering a wide range of temporal and spatial scales. Here, we study the scaling and statistical features of magnetic and electric field fluctuations below the ion-gyroperiod (i.e., in the dissipation domain) by carefully investigating the occurrence of local or global scaling features during a reconnection event studied by Eastwood et al . Our results point toward the presence of a global scale invariance, i.e., a mono-fractal nature, of fluctuations above the ion-cyclotron frequency and at spatial scales near the ion-inertial length.

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In-Situ Observations of Reconnection in Space

Cited by 176 publications

References 161 publications

What Controls the Structure and Dynamics of Earth’s Magnetosphere?

What Controls the Structure and Dynamics of Earth’s Magnetosphere?

Ideal MHD turbulence: the inertial range spectrum with collisionless dissipation

Statistical and Scaling Features of Fluctuations in the Dissipation Range During a Reconnection Event

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