Topics in Microphysics of Relativistic Plasmas

Lyutikov, Maxim; Lazarian, A.

doi:10.1007/s11214-013-9989-2

Cited by 14 publications

(14 citation statements)

References 94 publications

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“…We note that magnetar magnetospheres, even if they feature magnetizations exceeding σ cold e = 10 13 (Lyutikov & Lazarian 2013), support a very different reconnection regime due to pair and photon creations (Uzdensky 2011).…”

Section: Toward a New Regime: Non-dissipative Reconnection?mentioning

confidence: 80%

“…Such attributes made it attractive for high-energy astrophysics to explain, for example, radiation (Romanova & Lovelace 1992) and flares (Giannios et al 2009) in active galactic nuclei (AGNs) jets or in gamma-ray bursts (Lyutikov 2006a;Lazar et al 2009), the heating of AGN and microquasar coronae and associated flares (Di Matteo 1998;Merloni & Fabian 2001;Goodman & Uzdensky 2008;Reis & Miller 2013), the flat radio spectra from galactic nuclei and AGNs (Birk et al 2001), the heating of the lobes of giant radio galaxies (Kronberg et al 2004), the σ-paradox and particle acceleration at pulsar wind termination shocks (Kirk & Skjaeraasen 2003;Pétri & Lyubarsky 2007;Sironi & Spitkovsky 2011), GeV flares from the Crab nebula (Cerutti et al 2012a(Cerutti et al ,b, 2013, transient outflow production in microquasars and quasars (de Gouveia dal Pino & Lazarian 2005;de Gouveia Dal Pino et al 2010;Kowal et al 2011;Dexter et al 2014), gamma-ray burst outflows and non-thermal emissions (Drenkhahn & Spruit 2002;McKinney & Uzdensky 2012), X-ray flashes (Drenkhahn & Spruit 2002), soft gamma-ray repeaters (Lyutikov 2006b;Uzdensky 2011), flares in double pulsar systems (Lyutikov & Lazarian 2013), or energy extraction in the ergosphere of black holes (Koide & Arai 2008).…”

Section: Introductionmentioning

confidence: 99%

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Relativistic magnetic reconnection in collisionless ion-electron plasmas explored with particle-in-cell simulations

Melzani

Walder

Folini

et al. 2014

A&A

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Magnetic reconnection is a leading mechanism for magnetic energy conversion and high-energy non-thermal particle production in a variety of high-energy astrophysical objects, including ones with relativistic ion-electron plasmas (e.g., microquasars or AGNs), a regime where first principle studies are scarce. We present 2D particle-in-cell (PIC) simulations of low β ion-electron plasmas under relativistic conditions, i.e., with inflow magnetic energy exceeding the plasma restmass energy. We identify outstanding properties: (i) For relativistic inflow magnetizations (here 10 ≤ σ e ≤ 360), the reconnection outflows are dominated by thermal agitation instead of bulk kinetic energy. (ii) At high inflow electron magnetization (σ e ≥ 80), the reconnection electric field is sustained more by bulk inertia than by thermal inertia. It challenges the thermal-inertia paradigm and its implications. (iii) The inflows feature sharp transitions at the entrance of the diffusion zones. These are not shocks but results from particle ballistic motions, all bouncing at the same location, provided that the thermal velocity in the inflow is far lower than the inflow E × B bulk velocity. (iv) Island centers are magnetically isolated from the rest of the flow and can present a density depletion at their center. (v) The reconnection rates are slightly higher than in non-relativistic studies. They are best normalized by the inflow relativistic Alfvén speed projected in the outflow direction, which then leads to rates in a close range (0.14-0.25), thus allowing for an easy estimation of the reconnection electric field.

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Section: Toward a New Regime: Non-dissipative Reconnection?mentioning

confidence: 80%

Section: Introductionmentioning

confidence: 99%

Relativistic magnetic reconnection in collisionless ion-electron plasmas explored with particle-in-cell simulations

Melzani

Walder

Folini

et al. 2014

A&A

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“…The suggestion that LV99 is applicable to relativistic reconnection motivated the use of the model for explaining γ-ray bursts [36,119] and in accretion discs around black holes and pulsars [120,121]. Now, as the extension of the model to relativistic case has been confirmed, these and other cases where the relativistic analogue of LV99 process was discussed to be applicable [21] are given numerical support.…”

Section: (F) Relativistic Reconnectionmentioning

confidence: 95%

Turbulent reconnection and its implications

Lazarían¹,

Eyink

Vishniac

et al. 2015

Phil. Trans. R. Soc. A.

Self Cite

115

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“…In general, magnetic reconnection that does not necessarily result from having a striped-wind configuration has also been invoked in many works over the traditional internal-shock scenario to explain the prompt GRB emission due to it being more efficient in strongly magnetized flows (e.g. Thompson 1994;Lyutikov & Blandford 2003;Giannios & Spruit 2006;Lyutikov 2006;Zhang & Yan 2011).…”

Section: Introductionmentioning

confidence: 99%

“…Astrophysical plasmas near compact objects are inherently relativistic and collisionless (e.g. Lyutikov & Lazarian 2013), and they require some source of anomalous resistivity in order for reconnection to proceed. The rate of reconnection is set by the inflow velocity v in = β in c of the magnetized fluid into the current layer.…”

Section: Introductionmentioning

confidence: 99%

2D Relativistic MHD simulations of the Kruskal–Schwarzschild instability in a relativistic striped wind

Gill

Granot

Lyubarsky³

2017

Monthly Notices of the Royal Astronomical Society

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We study the linear and non-linear development of the Kruskal-Schwarzchild Instability in a relativisitically expanding striped wind. This instability is the generalization of Rayleigh-Taylor instability in the presence of a magnetic field. It has been suggested to produce a selfsustained acceleration mechanism in strongly magnetized outflows found in active galactic nuclei, gamma-ray bursts, and micro-quasars. The instability leads to magnetic reconnection, but in contrast with steady-state Sweet-Parker reconnection, the dissipation rate is not limited by the current layer's small aspect ratio. We performed two-dimensional (2D) relativistic magnetohydrodynamic (RMHD) simulations featuring two cold and highly magnetized (1 σ 10 3 ) plasma layers with an anti-parallel magnetic field separated by a thin layer of relativistically hot plasma with a local effective gravity induced by the outflow's acceleration. Our simulations show how the heavier relativistically hot plasma in the reconnecting layer drips out and allows oppositely oriented magnetic field lines to reconnect. The instability's growth rate in the linear regime matches the predictions of linear stability analysis. We find turbulence rather than an ordered bulk flow near the reconnection region, with turbulent velocities up to ∼ 0.1c, largely independent of model parameters. However, the magnetic energy dissipation rate is found to be much slower, corresponding to an effective ordered bulk velocity inflow into the reconnection region v in = β in c, of 10 −3 β in 5 × 10 −3 . This occurs due to the slow evacuation of hot plasma from the current layer, largely because of the Kelvin-Helmholtz instability experienced by the dripping plasma. 3D RMHD simulations are needed to further investigate the non-linear regime.

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Topics in Microphysics of Relativistic Plasmas

Cited by 14 publications

References 94 publications

Relativistic magnetic reconnection in collisionless ion-electron plasmas explored with particle-in-cell simulations

Relativistic magnetic reconnection in collisionless ion-electron plasmas explored with particle-in-cell simulations

Turbulent reconnection and its implications

2D Relativistic MHD simulations of the Kruskal–Schwarzschild instability in a relativistic striped wind

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