Observational Signatures of Particle Acceleration in Supernova Remnants

Helder, E. A.; Vink, Jacco; Bykov, A. M.; Ohira, Yutaka; Raymond, J. C.; Terrier, R.

doi:10.1007/978-1-4614-6455-6_12

Cited by 8 publications

(10 citation statements)

References 334 publications

(111 reference statements)

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“…A strong non-relativistic shock may transfer up to 10% of the ram pressure into magnetic fields as it is illustrated in the left panel of Figure 7. There are convincing observational evidences for strong non-adiabatic amplification of magnetic fields in the vicinities of forward shocks of a number of young SNRs including Cas A, Tycho, SN 1006, RXJ 1713.7-3946 and others obtained via arcsecond angular resolution imaging of synchrotron structures in these SNRs with Chandra (see, e.g., Vink 2012, Bamba et al 2005, Uchiyama et al 2007, Reynolds et al 2012, Helder et al 2012, Ressler et al 2014, Tananbaum et al 2014. The mechanisms of magnetic field amplification which are associated with CR-driven instabilities were thoroughly discussed and reviwed in Blandford and Eichler (1987), Bell and Lucek (2001), Malkov and Drury (2001), Zweibel (2003), Bell (2004), Lemoine and Pelletier (2010), Schure et al (2012), Blasi (2013), Bykov et al (2013a).…”

Section: Particle Acceleration By Collisionless Shocksmentioning

confidence: 93%

“…The high efficiency of particle acceleration which may be well above 10% as deduced, in particular, from observations of young supernova remnants (see, e.g., Vink 2012, Helder et al 2012, Blasi 2013 implies strong coupling between the accelerated particle population and the shock structure. The coupling is realized through the electromagnetic fluctuations carried with the shock flow and responsible for inelastic scattering the particles.…”

Section: Particle Acceleration By Collisionless Shocksmentioning

confidence: 98%

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Nonthermal particles and photons in starburst regions and superbubbles

Bykov

2014

Astron Astrophys Rev

110

100

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Starforming factories in galaxies produce compact clusters and loose associations of young massive stars. Fast radiation-driven winds and supernovae input their huge kinetic power into the interstellar medium in the form of highly supersonic and superalfvenic outflows. Apart from gas heating, collisionless relaxation of fast plasma outflows results in fluctuating magnetic fields and energetic particles. The energetic particles comprise a long-lived component which may contain a sizeable fraction of the kinetic energy released by the winds and supernova ejecta and thus modify the magnetohydrodynamic flows in the systems. We present a concise review of observational data and models of nonthermal emission from starburst galaxies, superbubbles, and compact clusters of massive stars. Efficient mechanisms of particle acceleration and amplification of fluctuating magnetic fields with a wide dynamical range in starburst regions are discussed. Sources of cosmic rays, neutrinos and multi-wavelength nonthermal emission associated with starburst regions including potential galactic "PeVatrons" are reviewed in the global galactic ecology context.

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Section: Particle Acceleration By Collisionless Shocksmentioning

confidence: 93%

Section: Particle Acceleration By Collisionless Shocksmentioning

confidence: 98%

Nonthermal particles and photons in starburst regions and superbubbles

Bykov

2014

Astron Astrophys Rev

110

100

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“…Helder et al 2012;Blasi 2013;Amato 2014). This association has gained important observational support in recent years thanks to the data collected by X-ray telescopes such as Chandra and XMM-Newton and gamma-ray telescopes such as Fermi and AGILE, with the former instruments showing accelerated electrons with energies up to tens of TeV (Reynolds et al 2012;) and the latter highlighting for the first time the presence of relativistic protons in SNRs (Abdo et al 2010a,b;Tavani et al 2010;Giuliani et al 2011).…”

Section: Superdi Usive Transport At Heliospheric Shocksmentioning

confidence: 99%

Superdiffusive transport in laboratory and astrophysical plasmas

et al. 2015

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In the last few years it has been demonstrated, both by data analysis and by numerical simulations, that the transport of energetic particles in the presence of magnetic turbulence can be superdiffusive rather than normal diffusive (Gaussian). The term 'superdiffusive' refers to the mean square displacement of particle positions growing superlinearly with time, as compared to the normal linear growth. The so-called anomalous transport, which in general comprises both subdiffusion and superdiffusion, has gained growing attention during the last two decades in many fields including laboratory plasma physics, and recently in astrophysics and space physics. Here we show a number of examples, both from laboratory and from astrophysical plasmas, where superdiffusive transport has been identified, with a focus on what could be the main influence of superdiffusion on fundamental processes like diffusive shock acceleration and heliospheric energetic particle propagation. For laboratory plasmas, superdiffusion appears to be due to the presence of electrostatic turbulence which creates long-range correlations and convoluted structures in perpendicular transport: this corresponds to a similar phenomenon in the propagation of solar energetic particles (SEPs) which leads to SEP dropouts. For the propagation of energetic particles accelerated at interplanetary shocks in the solar wind, parallel superdiffusion seems to be prevailing; this is based on a pitch-angle scattering process different from that envisaged by quasi-linear theory, and this emphasizes the importance of nonlinear interactions and trapping effects. In the case of supernova remnant shocks, parallel superdiffusion is possible at quasi-parallel shocks, as occurring in the interplanetary space, and perpendicular superdiffusion is possible at quasi-perpendicular shocks, as corresponding to Richardson diffusion: therefore, cosmic ray acceleration at supernova remnant shocks should be formulated in terms of superdiffusion. The possible relations among anomalous transport in laboratory, heliospheric, and astrophysical plasmas will be indicated.

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“…Recent observations of forward shocks in galactic SNRs indicate a substantial role of nonthermal components in the energy budgets of post-shock flows (e.g., Helder et al 2012). While the fraction of the energy dissipated in the shock itself may be smaller for slower radiative shocks, the enhanced radiative cooling in their post-shocks leads to stronger compression so that cosmic ray and magnetic pressure can dominate over thermal pressure in the zones where most of the observed optical and IR emission is produced.…”

Section: Introductionmentioning

confidence: 99%

“…Raymond et al (1988b) analyzed a shock in the Cygnus Loop SNR and found that the nonthermal pressure exceeds the thermal pressure by an order of magnitude in the zones where the [S II] lines are formed, though they were unable to distinguish between magnetic and cosmic ray contributions. Neutral particles could affect the processes of particle acceleration (e.g., Draine and McKee 1993;O'C Drury et al 1996;Malkov et al 2005;Blasi et al 2012;Inoue et al 2012;Ohira 2012;Helder et al 2012;Morlino et al 2012a), magnetic field amplification and plasma heating in the upstream region (e.g., Bykov and Toptygin 2005;Reville et al 2007).…”

Section: Introductionmentioning

confidence: 99%

Collisionless Shocks in Partly Ionized Plasma with Cosmic Rays: Microphysics of Non-thermal Components

Bykov

Malkov

Raymond

et al. 2013

Microphysics of Cosmic Plasmas

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In this review we discuss some observational aspects and theoretical models of astrophysical collisionless shocks in partly ionized plasma with the presence of nonthermal components. A specific feature of fast strong collisionless shocks is their ability to accelerate energetic particles that can modify the shock upstream flow and form the shock precursors. We discuss the effects of energetic particle acceleration and associated magnetic field amplification and decay in the extended shock precursors on the line and continuum multi-wavelength emission spectra of the shocks. Both Balmer-type and radiative astrophysical shocks are discussed in connection to supernova remnants interacting with partially neutral clouds. Quantitative models described in the review predict a number of observable line-like emission features that can be used to reveal the physical state of the matter in the shock precursors and the character of nonthermal processes in the shocks. Implications of recent progress of gamma-ray observations of supernova remnants in molecular clouds are highlighted.

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Observational Signatures of Particle Acceleration in Supernova Remnants

Cited by 8 publications

References 334 publications

Nonthermal particles and photons in starburst regions and superbubbles

Nonthermal particles and photons in starburst regions and superbubbles

Superdiffusive transport in laboratory and astrophysical plasmas

Collisionless Shocks in Partly Ionized Plasma with Cosmic Rays: Microphysics of Non-thermal Components

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