Charged Particle Diffusion in Isotropic Random Magnetic Fields

Subedi, Prachanda; Sonsrettee, W.; Blasi, Pasquale; Ruffolo, D.; Matthaeus, W. H.; Montgomery, David; Chuychai, P.; Dmitruk, P.; Wan, Minping; Parashar, T. N.; Chhiber, R.

doi:10.3847/1538-4357/aa603a

Cited by 63 publications

(62 citation statements)

References 55 publications

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“…As discussed in P18, the high rate of SN explosions in the SBN is likely to produce a high level of turbulence, which is expected to reflect in a small diffusion coefficient. A theory of diffusion in strong turbulence was developed by Subedi et al (2017): the transport in these conditions can be approximated with a diffusion coefficient that has a functional shape…”

Section: Cosmic Rays In Sbni and Associated Emissionmentioning

confidence: 99%

Contribution of starburst nuclei to the diffuse gamma-ray and neutrino flux

Peretti

Blasi

Aharonian

et al. 2020

Monthly Notices of the Royal Astronomical Society

102

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In nuclei of starburst galaxies, the combination of an enhanced rate of supernova explosions and a high gas density suggests that cosmic rays can be efficiently produced, and that most of them lose their energy before escaping these regions, resulting in a large flux of secondary products, including neutrinos. Although the flux inferred from an individual starburst region is expected to be well below the sensitivity of current neutrino telescopes, such sources may provide a substantial contribution to the diffuse neutrino flux measured by IceCube.Here we compute the gamma-ray and neutrino flux due to starburst galaxies based on a physical model of cosmic ray transport in a starburst nucleus, and accounting for the redshift evolution of the number density of starburst sources as inferred from recent measurements of the star formation rate. The model accounts for gammaray absorption both inside the sources and in the intergalactic medium. The latter process is responsible for electromagnetic cascades, which also contribute to the diffuse gamma-ray background at lower energies. The conditions for acceleration of cosmic ray protons up to energies exceeding ∼ 10 PeV in starburst regions, necessary for the production of PeV neutrinos, are investigated in a critical way. We show that starburst nuclei can account for the diffuse neutrino flux above ∼ 200 TeV, thereby producing 40% of the extragalactic diffuse gamma-ray background. Below ∼ 200 TeV, the flux from starburst appears to be somewhat lower than the observed one, where both the Galactic contribution and the flux of atmospheric neutrinos may account for the difference.

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Section: Cosmic Rays In Sbni and Associated Emissionmentioning

confidence: 99%

Contribution of starburst nuclei to the diffuse gamma-ray and neutrino flux

Peretti

Blasi

Aharonian

et al. 2020

Monthly Notices of the Royal Astronomical Society

102

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“…There have been many theoretical articles on energetic charged particle diffusion associated with interplanetary turbulence. Some more recent papers are Lazarian et al (2012), Le Roux et al (2015, Sun et al (2016), and Subedi et al (2017). We direct the interested reader to these papers and their references.…”

Section: Energetic Particle Cross-field Diffusionmentioning

confidence: 99%

A Review of Alfvénic Turbulence in High‐Speed Solar Wind Streams: Hints From Cometary Plasma Turbulence

et al. 2018

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Solar wind turbulence within high‐speed streams is reviewed from the point of view of embedded single nonlinear Alfvén wave cycles, discontinuities, magnetic decreases (MDs), and shocks. For comparison and guidance, cometary plasma turbulence is also briefly reviewed. It is demonstrated that cometary nonlinear magnetosonic waves phase‐steepen, with a right‐hand circular polarized foreshortened front and an elongated, compressive trailing edge. The former part is a form of “wave breaking” and the latter that of “period doubling.” Interplanetary nonlinear Alfvén waves, which are arc polarized, have a ~180° foreshortened front and with an elongated trailing edge. Alfvén waves have polarizations different from those of cometary magnetosonic waves, indicating that helicity is a durable feature of plasma turbulence. Interplanetary Alfvén waves are noted to be spherical waves, suggesting the possibility of additional local generation. They kinetically dissipate, forming MDs, indicating that the solar wind is partially “compressive” and static. The ~2 MeV protons can nonresonantly interact with MDs leading to rapid cross‐field (~5.5% Bohm) diffusion. The possibility of local (~1 AU) generation of Alfvén waves may make it difficult to forecast High‐Intensity, Long‐Duration AE Activity and relativistic magnetospheric electrons with great accuracy. The future Solar Orbiter and Solar Probe Plus missions should be able to not only test these ideas but to also extend our knowledge of plasma turbulence evolution.

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“…The spectrum provides a complete statistical description of a Gaussian random magnetic field, so it must also determine the corresponding cosmic ray diffusivity for a given energy of particle. The propagation of cosmic rays in an isotropic Gaussian random magnetic field (for which the probability distribution function of each vector component is Gaussian) has been the subject of many studies (Berezinskii et al 1990;Michalek & Ostrowski 1997;Giacalone & Jokipii 1999;Casse et al 2002;Schlickeiser 2002;Parizot 2004;Candia & Roulet 2004;DeMarco et al 2007;Globus et al 2008;Shalchi 2009;Plotnikov et al 2011;Harari et al 2014;Snodin et al 2016;Subedi et al 2017). However, radio (Gaensler et al 2011;Haverkorn & Spangler 2013), submillimeter (Zaroubi et al 2015) and neutral hydrogen (Heiles & Troland 2005; Kalberla & Kerp 2016) observations suggest that the magnetic field in the ISM is strongly non-Gaussian, spatially intermittent, and filamentary.…”

Section: Implementation Of Random Magnetic Fieldsmentioning

confidence: 99%

Relative distribution of cosmic rays and magnetic fields

Seta

Shukurov

Wood

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Synchrotron radiation from cosmic rays is a key observational probe of the galactic magnetic field. Interpreting synchrotron emission data requires knowledge of the cosmic ray number density, which is often assumed to be in energy equipartition (or otherwise tightly correlated) with the magnetic field energy. However, there is no compelling observational or theoretical reason to expect such tight correlation to hold across all scales. We use test particle simulations, tracing the propagation of charged particles (protons) through a random magnetic field, to study the cosmic ray distribution at scales comparable to the correlation scale of the turbulent flow in the interstellar medium ( 100 pc in spiral galaxies). In these simulations, we find that there is no spatial correlation between the cosmic ray number density and the magnetic field energy density. In fact, their distributions are approximately statistically independent. We find that low-energy cosmic rays can become trapped between magnetic mirrors, whose location depends more on the structure of the field lines than on the field strength.

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Charged Particle Diffusion in Isotropic Random Magnetic Fields

Cited by 63 publications

References 55 publications

Contribution of starburst nuclei to the diffuse gamma-ray and neutrino flux

Contribution of starburst nuclei to the diffuse gamma-ray and neutrino flux

A Review of Alfvénic Turbulence in High‐Speed Solar Wind Streams: Hints From Cometary Plasma Turbulence

Relative distribution of cosmic rays and magnetic fields

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