Magnetic Field Amplification in Supernova Remnants

Lazarían, A.

doi:10.3847/1538-4357/aa956b

Cited by 35 publications

(23 citation statements)

References 67 publications

(87 reference statements)

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“…This interaction also leads to the field amplification by a turbulent dynamo process in the upstream region (Beresnyak et al 2009;del Valle et al 2016). Indeed, Xu & Lazarian (2017) pointed out that the shock crossing time of the precursor length is large enough to lead to full development of the precursor dynamo in partially ionized ISM. Note that the Balmer line emissions from Tycho's SNR indicate the interaction between the shock and the partially ionized ISM (e.g.…”

Section: Discussionmentioning

confidence: 99%

Discovery of Kolmogorov-like magnetic energy spectrum in Tycho’s supernova remnant by two-point correlations of synchrotron intensity

Shimoda

Akahori

Lazarian³

et al. 2018

Monthly Notices of the Royal Astronomical Society

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The spectral slope of the magnetic energy in supernova remnants (SNRs) can be obtained by analysis of spatial two-point correlation functions of synchrotron intensities. This method has been originally developed for the analysis of magnetic field structure in diffuse interstellar medium and applied when the geometry of the emission region is simple and known. In this paper, applying this correlation analysis to Tycho's SNR, for which the synchrotron emission region is known to be a spherical shell, we find that the magnetic energy spectrum shows the Kolmogorov-like scaling. Our results can be explained by turbulence developed downstream of the shock front via Richtmyer-Meshkov instability or an amplification of upstream magnetic field induced by cosmic rays. They could be discriminated by future observations with a sub arcsecond resolution such as Square Kilometer Array.

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Section: Discussionmentioning

confidence: 99%

Discovery of Kolmogorov-like magnetic energy spectrum in Tycho’s supernova remnant by two-point correlations of synchrotron intensity

Shimoda

Akahori

Lazarian³

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…Turbulent amplification via small-scale dynamo effects is perhaps another possibility. It can operate either in the precursor of the shock (del Valle et al 2016) or in the postshock region (Xu & Lazarian 2017). Amplifications from one to more than three orders of magnitude have been achieved with this mechanism for different setups of initial conditions.…”

Section: Stretching the Limitsmentioning

confidence: 99%

Particle acceleration in the superwinds of starburst galaxies

Romero

Müller

Roth

2018

A&A

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Context. Starbursts are galaxies undergoing massive episodes of star formation. The combined effect of stellar winds from hot stars and supernova explosions creates a high-temperature cavity in the nuclear region of these objects. The very hot gas expands adiabatically and escapes from the galaxy creating a superwind which sweeps matter from the galactic disk. The superwind region in the halo is filled with a multi-phase gas with hot, warm, cool, and relativistic components.Aims. The shocks associated with the superwind of starbursts and the turbulent gas region of the bubble inflated by them might accelerate cosmic rays up to high energies. In this work we calculate the cosmic ray production associated with the superwind using parameters that correspond to the nearby southern starburst galaxy NGC 253, which has been suggested as a potential accelerator of ultra-high-energy cosmic rays. Methods. We evaluate the efficiency of both diffusive shock acceleration (DSA) and stochastic diffusive acceleration (SDA) in the superwind of NGC 253. We estimate the distribution of both hadrons and leptons and calculate the corresponding spectral energy distributions of photons. The electromagnetic radiation can help to discriminate between the different scenarios analyzed. Results. We find that the strong mass load of the superwind, recently determined through ALMA observations, strongly attenuates the efficiency of DSA in NGC 253, whereas SDA is constrained by the age of the starburst. Conclusions. We conclude that NGC 253 and similar starbursts can only accelerate iron nuclei beyond ∼ 10 18 eV under very special conditions. If the central region of the galaxy harbors a starved supermassive black hole of ∼ 10 6 M , as suggested by some recent observations, a contribution in the range 10 18 − 10 19 eV can be present for accretion rateṡ m ∼ 10 −3 in Eddington units. Shock energies of the order of 100 EeV might only be possible if very strong magnetic field amplification occurs close to the superwind.

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“…The CSM could be highly turbulent and magnetized, because the violent CSM eruptions may also be accompanied by shocks (Murase et al 2014). The CSM may also be highly clumpy (Smith et al 2009), in which the turbulent dynamo process could amplify both upstream and downstream fields (e.g., Xu & Lazarian 2017). The upstream magnetic field amplification with ǫ B ∝ ǫ p M −1 A (where M A is the Alfvénic Mach number) could also be realized by CRs themselves via streaming instabilities (Caprioli & Spitkovsky 2014b).…”

Section: Introductionmentioning

confidence: 99%

High-energy Emission from Interacting Supernovae: New Constraints on Cosmic-Ray Acceleration in Dense Circumstellar Environments

Murase

Franckowiak

Maeda

et al. 2019

ApJ

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Supernovae (SNe) with strong interactions with circumstellar material (CSM) are promising candidate sources of high-energy neutrinos and gamma rays, and have been suggested as an important contributor to Galactic cosmic rays beyond 10 15 eV. Taking into account the shock dissipation by a fast velocity component of SN ejecta, we present comprehensive calculations of the non-thermal emission from SNe powered by shock interactions with a dense wind or CSM. Remarkably, we consider electromagnetic cascades in the radiation zone and subsequent attenuation in the pre-shock CSM. A new time-dependent phenomenological prescription provided by this work enables us to calculate gamma-ray, hard X-ray, radio, and neutrino signals, which originate from cosmic rays accelerated by the diffusive shock acceleration mechanism. We apply our results to SN IIn 2010jl and SN Ib/IIn 2014C, for which the model parameters can be determined from the multi-wavelength data. For SN 2010jl, the more promising case, by using the the latest Fermi Large Area Telescope (LAT) Pass 8 data release, we derive new constraints on the cosmic-ray energy fraction, ǫ p ∼ < 0.05 − 0.1. We also find that the late-time radio data of these interacting SNe are consistent with our model. Further multimessenger and multi-wavelength observations of nearby interacting SNe should give us new insights into the diffusive shock acceleration in dense environments as well as pre-SN mass-loss mechanisms.

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Magnetic Field Amplification in Supernova Remnants

Cited by 35 publications

References 67 publications

Discovery of Kolmogorov-like magnetic energy spectrum in Tycho’s supernova remnant by two-point correlations of synchrotron intensity

Discovery of Kolmogorov-like magnetic energy spectrum in Tycho’s supernova remnant by two-point correlations of synchrotron intensity

Particle acceleration in the superwinds of starburst galaxies

High-energy Emission from Interacting Supernovae: New Constraints on Cosmic-Ray Acceleration in Dense Circumstellar Environments

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