Small-scale turbulent dynamo in astrophysical environments: nonlinear dynamo and dynamo in a partially ionized plasma

Lazarían, A.

doi:10.1007/s41614-021-00051-3

Cited by 6 publications

(4 citation statements)

References 79 publications

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“…A review of astrophysical dynamos covering the era before 2005 is given by Brandenburg & Subramanian (2005a). Regarding small-scale turbulent dynamos in partially ionized plasmas, we refer to the recent review by Xu & Lazarian (2021). We also recommend the reviews by Crutcher (2012), Hennebelle & Inutsuka (2019), and Pattle et al (2022) on ISM magnetic fields.…”

Section: Introductionmentioning

confidence: 99%

Galactic Dynamos

Brandenburg¹,

Ntormousi²

2022

Preprint

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Spiral galaxies, including the Milky Way, have large-scale magnetic fields with significant energy densities. The dominant theory attributes these magnetic fields to a large-scale dynamo. We review the current status of dynamo theory and discuss various numerical simulations designed to explain either particular aspects of the problem or to reproduce galactic magnetic fields globally. Our main conclusions can be summarized as follows.

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Section: Introductionmentioning

confidence: 99%

Galactic Dynamos

Brandenburg¹,

Ntormousi²

2022

Preprint

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“…2) shows a ratio ( ★ )/ 0 1.35 that leads to 0 (0.1) = 2.5, with 0 (0.1) = 0 /0.1 mG. Such a relatively high 0 confirms that an amplification in W3 likely took place at the inward shock prior to year 2000, possibly via vorticity generation within the shocked layer due to the corrugation of the inward shock or an alternative mechanism [14].…”

Section: Flux Decreasementioning

confidence: 89%

Unfolding of the vortical amplification of the magnetic field at inward shocks of Supernova remnant Cassiopeia A

Fraschetti¹,

Katsuda²,

Sato³

et al. 2021

Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)

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We present an interpretation of the time variability of the -ray flux reported from a 15 years multi-epoch observational campaign of the supernova remnant Cassiopeia A by Chandra. The increase of the [4.2 − 6] keV non-thermal flux up to 50% is shown quantitatively to trace the growth of the magnetic field due to vortical amplification mechanism at inward shocks colliding with inner overdensities. The fast synchrotron cooling as compared with shock-acceleration time scale qualitatively explains the subsequent flux decrease.

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“…In the first group, magnetic fields are amplified on scales larger than the outer scale of turbulence in seconds on smaller scales [41]. In the second group, the small-scale turbulent dynamo is responsible for amplifying magnetic fields on scales smaller than the driving scale of turbulence in diverse astrophysical media [42].…”

Section: Mhd Turbulence and Dynamomentioning

confidence: 99%

Outlook on Magnetohydrodynamical Turbulence and Its Astrophysical Implications

Попова

Lazarian

2023

Fluids

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Magnetohydrodynamical (MHD) turbulence is ubiquitous in magnetized astrophysical plasmas, and it radically changes a great variety of astrophysical processes. In this review, we introduce the concept of MHD turbulence and explain the origin of its scaling. We consider the implications of MHD turbulence for various problems: dynamo in different types of stars, flare activity, solar and stellar wind from different stars, the propagation of cosmic rays, and star formation. We also discuss how the properties of MHD turbulence provide a new means of tracing magnetic fields in interstellar and intracluster media.

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Small-scale turbulent dynamo in astrophysical environments: nonlinear dynamo and dynamo in a partially ionized plasma

Cited by 6 publications

References 79 publications

Galactic Dynamos

Galactic Dynamos

Unfolding of the vortical amplification of the magnetic field at inward shocks of Supernova remnant Cassiopeia A

Outlook on Magnetohydrodynamical Turbulence and Its Astrophysical Implications

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