Frequent EUV microflashes at solar plume bases, each releasing ~10^24 erg, are identified as a new unipolar network event and suggested as a candidate mechanism to power the open corona and solar wind.
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Parker, Astrophys
18 Pith papers cite this work. Polarity classification is still indexing.
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A forward-modeling correction using real-time lens imaging reduces dust stray-light noise by 67% and restores expected coronal intensity profiles in ground-based data.
Young sub-Neptunes transition from core-powered bolometric escape to photoevaporative escape at smaller radii for lower-mass and more irradiated planets, with self-consistent simulations yielding combined mass-loss rates and analytic transition scalings.
A new source alignment technique applied to PSP and SO data reveals the solar wind speed increases by an average of 45% per radial decade between the spacecraft, indicating ongoing acceleration beyond 15 solar radii.
Misaligned protostellar cores produce a spiral flow outflow in addition to the disk wind, with the spiral flow becoming dominant and more massive at misalignment angles of 60 degrees or greater.
An optimization algorithm determines the optimal source surface radius for PFSS models by minimizing MSE against PSP radial field data from encounters 1-19 after backmapping, yielding increasing R_ss from solar minimum into cycle 25 ascending phase with improved open flux agreement.
A covariant first-principles reformulation of the Expanding Box Model treats solar wind expansion as an anisotropic spacetime metric, eliminating prior mathematical artifacts and recovering observed scalings.
Solar wind composition depends strongly on source distance from the open-closed boundary, with enhanced variability and slow-wind signatures concentrated within ~25 Mm of the boundary.
Numerical tracing of stochastic Parker spirals yields an angular field line spread of ~25° at 1 AU that narrows to ~4° when integrated backward to the solar source surface at 0.25 AU.
MHD simulation of a CME reveals that spacecraft connect to different regions of an inhomogeneous shock, reproducing the observed SEP flux differences among Earth, STA, and SolO.
Polytropic stellar wind models are extended beyond extreme adiabatic cases to non-adiabatic localized heating, with added energy shown plausible relative to flares and relevant to solar wind observations.
Oblique shocks in massive star clusters accelerate cosmic rays to multi-PeV energies, reproducing the LHAASO-observed knee as a sequence of rigidity-dependent cutoffs from combined supernova and wind shocks.
CIRs form closer to young fast-rotating solar-mass stars, migrate outward as rotation slows, and produced 10^3 to 10^7 times more energetic particles than today during the Hadean period.
No bursty planet-induced radio emission detected from five inactive M dwarfs; upper limits constrain GJ 367 b magnetosphere to <0.8 G under assumed stellar wind conditions.
Long-term near-Earth solar wind observations establish a robust empirical connection between flow speed and magnetohydrodynamic turbulence energy.
Adapts FLASH code for MHD rigid body simulations to model non-magnetized planet-stellar wind interactions and examine viscosity influence on flow patterns.
Detection and characterization of two eccentric warm Jupiters TOI-2147 b (P=26.2 d, e=0.29, M=116 M⊕) and TOI-6019 b (P=14.5 d, e=0.48, M=149 M⊕) with TESS and MaHPS data, showing mildly inflated radii consistent with tidal heating.
This review summarizes the basic principles of electron transport in inhomogeneous and tangled magnetic fields through gyro-centre trajectories, kinetic instabilities, trapping, and diffusion processes.
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A robust empirical relationship between speed and turbulence energy in the near-Earth solar wind
Long-term near-Earth solar wind observations establish a robust empirical connection between flow speed and magnetohydrodynamic turbulence energy.