Notes on Magnetohydrodynamics of Magnetic Reconnection in Turbulent Media

Browning, Philippa; Lazarían, A.

doi:10.1007/978-1-4899-7413-6_10

Cited by 7 publications

(8 citation statements)

References 150 publications

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“…As a result, the central part of the exhaust is minimally affected by the background solar wind turbulence while the near edge portion of plasma could be disturbed. However, as pointed by Browning and Lazarian 36 , the couple between microscale kinetic effects and macroscale turbulence generated by reconnection remains an open question.…”

Section: Discussionmentioning

confidence: 99%

Direct evidence for kinetic effects associated with solar wind reconnection

Wang

Wei

et al. 2015

Sci Rep

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Kinetic effects resulting from the two-fluid physics play a crucial role in the fast collisionless reconnection, which is a process to explosively release massive energy stored in magnetic fields in space and astrophysical plasmas. In-situ observations in the Earth's magnetosphere provide solid consistence with theoretical models on the point that kinetic effects are required in the collisionless reconnection. However, all the observations associated with solar wind reconnection have been analyzed in the context of magnetohydrodynamics (MHD) although a lot of solar wind reconnection exhausts have been reported. Because of the absence of kinetic effects and substantial heating, whether the reconnections are still ongoing when they are detected in the solar wind remains unknown. Here, by dual-spacecraft observations, we report a solar wind reconnection with clear Hall magnetic fields. Its corresponding Alfvenic electron outflow jet, derived from the decouple between ions and electrons, is identified, showing direct evidence for kinetic effects that dominate the collisionless reconnection. The turbulence associated with the exhaust is a kind of background solar wind turbulence, implying that the reconnection generated turbulence has not much developed.

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Section: Discussionmentioning

confidence: 99%

Direct evidence for kinetic effects associated with solar wind reconnection

Wang

Wei

et al. 2015

Sci Rep

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“…The turbulent reconnection has shown promise in explaining various astrophysical problems, as well as in addressing problems facing solar physics and heliospheric research. Some of these are discussed in this review, while others are discussed in specialized reviews [21,153,181].…”

Section: (E) Present State Of Turbulent Reconnection Theory and Outst...mentioning

confidence: 99%

Turbulent reconnection and its implications

Lazarían¹,

Eyink

Vishniac

et al. 2015

Phil. Trans. R. Soc. A.

115

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“…Moreover, it is worth to note that the process which is responsible for changes of the magnetic field topology is a turbulent magnetic reconnection (e.g. [14]). For this process Parker [15] and Sweet [16] have proposed independently the first analytical model-when strong magnetic field lines diffuse through the plasma then reconnection can occur.…”

Section: Pos(icrc2017)030 Pos(icrc2017)030mentioning

confidence: 99%

α-ω effect and recurrent changes of galactic cosmic rays intensity

Gil¹,

Alania²

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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We recognize a quasi-recurrence with duration of 3 to 4 Carrington rotations period (3-4 CRP) in changes of amplitudes of the 27-day variation of galactic cosmic rays (GCR) intensity, solar activity (SA) and solar wind (SW) parameters, as well. We attribute this phenomenon to the presence of a spatial topological structure (STS) of the solar magnetic field. STS is created by α-ω effect in the inner solar atmosphere, from photosphere to lower corona. STS exists due to the asymmetry of solar dynamo and solar differential rotation. Studying this phenomenon by the aid of spectral analysis methods we found an existence of the quasi-periodicities with the duration shorter than, and longer than the 3-4 CRP. This 3-4 CRP quasi-periodicity mode corresponds to the extreme interval ∆t of differential rotation periods, ∆t = 35 days-25 days (from poles to equator of the Sun, respectively). We assume also that the process like to α-ω appears in time intervals corresponding to the transitional differential rotation periods, as well, e.g. ∆t1 = 26 days-25 days, ∆t2 = 27 days-25 days, and so forth, to ∆t = 35 days-25 days. We assume that extensive range of quasi-periodicities of GCR intensity, SW and SA parameters can be related to the combined influence of turbulent solar dynamo and solar differential rotation. Thus, STS should be very complex pattern containing a broad modes of oscillations responsible for various types of quasiperiodicities. So, we believe that it is possible to find an evidence that any alternation: periodical or nonperiodical in GCR intensity and in parameters of solar activity and solar wind is strongly related with temporal changes of the various scales of STS.

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Notes on Magnetohydrodynamics of Magnetic Reconnection in Turbulent Media

Cited by 7 publications

References 150 publications

Direct evidence for kinetic effects associated with solar wind reconnection

Direct evidence for kinetic effects associated with solar wind reconnection

Turbulent reconnection and its implications

α-ω effect and recurrent changes of galactic cosmic rays intensity

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