Energy-dependent polarization angle variability distinguishes reconnection from turbulence as the driver of blazar flares, with Mrk 421 and 1ES 1959+650 data favoring reconnection.
Mixed citations
Title resolution pending
Mixed citation behavior. Most common role is background (67%).
10
Pith papers citing it
158
external citations · Crossref
Background
67% of classified citations
citation-role summary
background 5
method 1
citation-polarity summary
years
2026 10verdicts
UNVERDICTED 10representative citing papers
Anisotropic low-energy electron pitch angles reduce synchrotron polarization degrees in gamma-ray and X-ray bands of GRB prompt emission compared to isotropic cases, with optical band behavior depending on the slope m, offering a possible match to some observations.
In multispecies relativistic turbulence, energization occurs at reconnection current sheets driven by the divergence of the relativistic pressure tensor, with electrons accelerated more efficiently than positrons due to species imbalance.
A population of AGN coronae with magnetization parameters spanning up to σ ~ 10 can reproduce the entire observed diffuse neutrino flux from TeV to PeV energies.
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.
Reconnection in transrelativistic AGN coronae can energize protons to tens of PeV, producing a neutrino spectrum consistent with NGC 1068 observations without tuning the proton spectral slope.
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).
Entity PIC code updated with up to 11th-order current deposit and generalized field stencils, with tests showing improved conservation properties and suppression of numerical effects.
A model of accretion-disk dynamos as synchronized macro-spins unifies broadband variability, coronal heating, jets, and hard/soft cycles via collective spin dynamics.
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
-
Energy-Dependent Polarization Angle Variability as a Robust Diagnostic for Blazar Flaring Mechanisms
Energy-dependent polarization angle variability distinguishes reconnection from turbulence as the driver of blazar flares, with Mrk 421 and 1ES 1959+650 data favoring reconnection.
-
Synchrotron polarization of anisotropic electron distribution in GRB prompt emission
Anisotropic low-energy electron pitch angles reduce synchrotron polarization degrees in gamma-ray and X-ray bands of GRB prompt emission compared to isotropic cases, with optical band behavior depending on the slope m, offering a possible match to some observations.
-
Particle-acceleration mechanisms in multispecies relativistic plasmas
In multispecies relativistic turbulence, energization occurs at reconnection current sheets driven by the divergence of the relativistic pressure tensor, with electrons accelerated more efficiently than positrons due to species imbalance.
-
Turbulent AGN coronae as the origin of diffuse neutrinos up to PeV energies
A population of AGN coronae with magnetization parameters spanning up to σ ~ 10 can reproduce the entire observed diffuse neutrino flux from TeV to PeV energies.
-
Guide-Field-mediated Multiscale Instabilities in Relativistic Reconnection
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.
-
Can magnetic reconnection power neutrino emission from AGN coronae?
Reconnection in transrelativistic AGN coronae can energize protons to tens of PeV, producing a neutrino spectrum consistent with NGC 1068 observations without tuning the proton spectral slope.
-
Distributions of particles accelerated by strong Alfv\'enic turbulence
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).
-
Entity -- Hardware-agnostic Particle-in-Cell Code for Plasma Astrophysics. III: Higher-order shape functions & generalized field stencils
Entity PIC code updated with up to 11th-order current deposit and generalized field stencils, with tests showing improved conservation properties and suppression of numerical effects.
-
A Synchronized Spin Model for Black-Hole Accretion Systems
A model of accretion-disk dynamos as synchronized macro-spins unifies broadband variability, coronal heating, jets, and hard/soft cycles via collective spin dynamics.
-
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.