First multipoint L1 observations reveal spatially varying MHD turbulence with strong anisotropies, shock-modified sheath regions, and compressible signatures in the October 2024 ICME.
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2: Strong alfvenic turbulence
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EHT data show a 51.8 microarcsecond ring around Sgr A* consistent with the shadow of a 4 million solar mass Kerr black hole viewed at moderate inclination.
In magnetically dominated relativistic collisionless plasmas, Alfvén and slow modes follow anisotropic Goldreich-Sridhar scaling, fast modes are isotropic with larger kinetic energy fraction, and dynamic alignment weakens near kinetic scales due to thermal fluctuations.
MMS data from a 2023 CME show elevated electron temperatures with superthermal tails, depleted mid-energy electrons, and weak MHD-like turbulence with reduced intermittency in the rare sub-Alfvénic solar wind at 1 AU.
Turbulent electron-ion coronae around accreting black holes self-regulate into a two-temperature state that generates nonthermal ions and X-ray spectra consistent with observations including an MeV tail.
Three-dimensional three-temperature simulations of colliding supersonic plasma flows from irradiated CH mesh targets produce a persistent shocked turbulent mixing layer that evolves toward an isothermal state with anisotropic Reynolds stress and effective Reynolds number around 200.
Observational study of MBM12 shows CO-to-H2 conversion factor near galactic average with density-dependent variations, high virial parameters decreasing at small scales, broken power-law mass-size relations indicating external pressure, and magnetic field orientation transition at N(H2) = 4.5e21 cm-
Simulations demonstrate non-monotonic guide-field regulation of reconnection efficiency via balance between drift-kink suppression and tearing-mode hindrance in 3D relativistic current sheets.
Curvature acceleration in strong Alfvénic turbulence saturates due to diminishing energy exchange efficiency, producing particle distributions f(p) ∝ p^{-3} (non-relativistic) and f(γ) ∝ γ^{-3} (ultrarelativistic).
Observational modeling of GWA and LAB survey spectra yields 19.8% CNM, 32.5% UNM and 47.8% WNM, in agreement with the TIGRESS-NCR simulation under fixed spin-temperature boundaries.
A review summarizing pitfalls in older CR-MHD models and progress toward more rigorous treatments that connect microphysical CR scales to galactic dynamics.