Particle Acceleration in Shearing Flows: Efficiencies and Limits

Rieger, F.; Duffy, P.

doi:10.3847/2041-8213/ab563f

Cited by 36 publications

(36 citation statements)

References 39 publications

(52 reference statements)

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“…Another point not considered in this work is the particle acceleration and the non-thermal processes: particles can be accelerated at magnetic reconnections (Giannios 2010;Giannios et al 2009;McKinney & Uzdensky 2012;Melzani et al 2014) and shocks (Araudo et al 2009;Bordas et al 2009;de la Cita et al 2017) or by stochastic interaction with magnetized turbulence. Shearing flow acceleration as also been invoked as potential injection process of relativistic particles (Rieger & Duffy 2019). An extensive review of such processes is given in Marcowith et al (2020).…”

Section: Non-thermal Components and Radiative Processes Emissionmentioning

confidence: 99%

Effects of radiative losses on the relativistic jets of high-mass microquasars

Charlet,

Walder,

Marcowith

et al. 2021

Preprint

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Context. Relativistic jets are ubiquitous in astrophysics. High Mass Microquasars (HMMQs) are useful labs to study such jets, as they are relatively close and evolve over observable time scales. The ambient medium into which the jet propagates is, however, far from homogeneous. Corresponding simulation studies to date consider various forms of a wind-shaped ambient medium but typically neglect radiative cooling and relativistic effects. Aims. We investigate the dynamical and structural effects of radiative losses and system parameters on relativistic jets in HMMQs, from the jet launch to its propagation over several tens of orbital separations. Methods. We use 3D relativistic hydrodynamical simulations including parameterized radiative cooling derived from relativistic thermal plasma distribution to carry out parameter studies around two fiducial cases inspired by Cygnus X-1 and Cygnus X-3. Results. Radiative losses are found to be more relevant in Cygnus X-3 than Cygnus X-1. Varying jet power, jet temperature, or the wind of the donor star tends to have a larger impact at early times, when the jet forms and instabilities initially develop, than at later times when the jet has reached a turbulent state. Conclusions. Radiative losses may be dynamically and structurally relevant at least in Cygnus X-3 case, and thus should be examined in more detail.

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Section: Non-thermal Components and Radiative Processes Emissionmentioning

confidence: 99%

Effects of radiative losses on the relativistic jets of high-mass microquasars

Charlet,

Walder,

Marcowith

et al. 2021

Preprint

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“…The multiwavelength emission of AGN requires a mechanism able to reaccelerate particles as they travel along the jet (Blandford & Koenigl 1979). The processes that are most frequently proposed are acceleration from internal shocks (Pelletier et al 2019; Movies are available at https://www.aanda.org 2019a,b), shear acceleration (Rieger & Duffy 2019;Tavecchio 2021), or magnetic reconnection (Blandford et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Flux variability from ejecta in structured relativistic jets with large-scale magnetic fields

Clairfontaine

Méliani

Zech

et al. 2021

A&A

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Context. Standing and moving shocks in relativistic astrophysical jets are very promising sites for particle acceleration to large Lorentz factors and for the emission from the radio up to the γ-ray band. They are thought to be responsible for at least part of the observed variability in radio-loud active galactic nuclei. Aims. We aim to simulate the interactions of moving shock waves with standing recollimation shocks in structured and magnetized relativistic jets and to characterize the profiles of connected flares in the radio light curve. Methods. Using the relativistic magneto-hydrodynamic code MPI-AMRVAC and a radiative transfer code in post-processing, we explore the influence of the magnetic-field configuration and transverse stratification of an over-pressured jet on its morphology, on the moving shock dynamics, and on the emitted radio light curve. First, we investigate different large-scale magnetic fields with their effects on the standing shocks and on the stratified jet morphology. Secondly, we study the interaction of a moving shock wave with the standing shocks. We calculated the synthetic synchrotron maps and radio light curves and analyze the variability at two frequencies 1 and 15.3 GHz and for several observation angles. Finally, we compare the characteristics of our simulated light curves with radio flares observed from the blazar 3C 273 with the Owens Valley Radio Observatory and Very Long Baseline Array in the MOJAVE survey between 2008 and 2019. Results. We find that in a structured over-pressured relativistic jet, the presence of the large-scale magnetic field structure changes the properties of the standing shock waves and leads to an opening in the jet. The interaction between waves from inner and outer jet components can produce strong standing shocks. When crossing such standing shocks, moving shock waves accompanying overdensities injected in the base of the jet cause very luminous radio flares. The observation of the temporal structure of these flares under different viewing angles probes the jet at different optical depths. At 1 GHz and for small angles, the self-absorption caused by the moving shock wave becomes more important and leads to a drop in the observed flux after it interacts with the brightest standing knot. A weak asymmetry is seen in the shape of the simulated flares, resulting from the remnant emission of the shocked standing shocks. The characteristics of the simulated flares and the correlation of peaks in the light curve with the crossing of moving and standing shocks favor this scenario as an explanation of the observed radio flares of 3C 273.

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“…Other instabilities such as the kinetic Kelvin-Helmholtz (kKHI) and the Mushroom Instability (MI) are driven by the shear velocity at the boundary between the jet and the ambient medium. These instabilities also contribute to the acceleration of particles [32]. As a rule of thumb, kKHI is generated along the jet's velocity.…”

Section: Particle-in-cell Approach and Plasma Instabilitiesmentioning

confidence: 99%

Particle-in-Cell Simulations of Astrophysical Relativistic Jets

Meli

Nishikawa

2021

Universe

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Astrophysical relativistic jets in active galactic nuclei, gamma-ray bursts, and pulsars is the main key subject of study in the field of high-energy astrophysics, especially regarding the jet interaction with the interstellar or intergalactic environment. In this work, we review studies of particle-in-cell simulations of relativistic electron–proton (e−−p+) and electron–positron (e±) jets, and we compare simulations that we have conducted with the relativistic 3D TRISTAN-MPI code for unmagnetized and magnetized jets. We focus on how the magnetic fields affect the evolution of relativistic jets of different compositions, how the jets interact with the ambient media, how the kinetic instabilities such as the Weibel instability, the kinetic Kelvin–Helmholtz instability and the mushroom instability develop, and we discuss possible particle acceleration mechanisms at reconnection sites.

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Particle Acceleration in Shearing Flows: Efficiencies and Limits

Cited by 36 publications

References 39 publications

Effects of radiative losses on the relativistic jets of high-mass microquasars

Effects of radiative losses on the relativistic jets of high-mass microquasars

Flux variability from ejecta in structured relativistic jets with large-scale magnetic fields

Particle-in-Cell Simulations of Astrophysical Relativistic Jets

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