Advection-only galactic wind models fail to reproduce observed vertical radio profiles without unrealistic velocities, synchrotron spectra are biased toward young electrons in dense regions, and bremsstrahlung/Coulomb losses cannot be neglected even when subdominant.
Caprioli \ and\ author A
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Cosmic rays enhance momentum transfer in Kelvin-Helmholtz turbulent shear flows by acting as long-range messengers when their gyroradii are smaller than the shear scale, increasing effective viscosity even when not energetically dominant.
Ion injection at perpendicular shocks requires 3D geometry to capture the porosity of downstream magnetic turbulence that lets particles return upstream and gain energy.
VLA L-band polarization observations of SNR G7.7-3.7 show cocoon morphology from interaction with pre-existing circumstellar shells, with magnetic fields compressed along filaments and RM variations tracing massive progenitor winds.
Hybrid simulations of the ion Weibel instability require a minimum grid resolution that scales with Alfvénic Mach number to correctly reproduce magnetic-field growth and saturation without introducing unphysical whistler modes.
A two-component Galactic source model with supernova remnants below 100 TeV and microquasars above, using charge-dependent cutoffs, accounts for cosmic-ray spectra, composition, and the all-particle spectrum up to PeV energies while ruling out nuclei-dependent cutoffs.
Coherent structures that self-consistently emerge in strong MHD turbulence serve as the dominant sites for localized electric-field intensification and repeated particle acceleration across cosmic plasmas.
citing papers explorer
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Revisiting radio synchrotron diagnostics in star-forming galaxies
Advection-only galactic wind models fail to reproduce observed vertical radio profiles without unrealistic velocities, synchrotron spectra are biased toward young electrons in dense regions, and bremsstrahlung/Coulomb losses cannot be neglected even when subdominant.
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Hybrid Simulations of Supersonic Shear Flows: II) Cosmic Ray Viscosity
Cosmic rays enhance momentum transfer in Kelvin-Helmholtz turbulent shear flows by acting as long-range messengers when their gyroradii are smaller than the shear scale, increasing effective viscosity even when not energetically dominant.
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The role of three-dimensional effects on ion injection and acceleration in perpendicular shocks
Ion injection at perpendicular shocks requires 3D geometry to capture the porosity of downstream magnetic turbulence that lets particles return upstream and gain energy.
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The Cocoon from a Massive Star's Death: VLA Radio Polarization Study of Possible Historical Supernova Remnant G7.7$-$3.7
VLA L-band polarization observations of SNR G7.7-3.7 show cocoon morphology from interaction with pre-existing circumstellar shells, with magnetic fields compressed along filaments and RM variations tracing massive progenitor winds.
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Ion Weibel Instability in the hybrid framework: the optimal resolution
Hybrid simulations of the ion Weibel instability require a minimum grid resolution that scales with Alfvénic Mach number to correctly reproduce magnetic-field growth and saturation without introducing unphysical whistler modes.
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Two kinds of Galactic source populations could explain the cosmic-ray observation up to the "knee" region
A two-component Galactic source model with supernova remnants below 100 TeV and microquasars above, using charge-dependent cutoffs, accounts for cosmic-ray spectra, composition, and the all-particle spectrum up to PeV energies while ruling out nuclei-dependent cutoffs.
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Strong MHD Turbulence and Coherent Structures as Drivers of Cosmic Particle Acceleration
Coherent structures that self-consistently emerge in strong MHD turbulence serve as the dominant sites for localized electric-field intensification and repeated particle acceleration across cosmic plasmas.
- On The Nonthermal Power Laws In Magnetized Turbulent Plasmas