{"total":10,"items":[{"citing_arxiv_id":"2607.02044","ref_index":221,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Energetic particle-mediated interplanetary shocks observed by Solar Orbiter","primary_cat":"physics.space-ph","submitted_at":"2026-07-02T11:12:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Four Solar Orbiter interplanetary shocks show energetic particle pressure dominating upstream, indicating particle-mediated modification of collisionless shocks.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.31433","ref_index":32,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A new model for long-term forecasting of Galactic cosmic rays","primary_cat":"physics.space-ph","submitted_at":"2026-06-30T10:00:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A 1D spherically symmetric Parker transport model with charge-sign and rigidity-dependent parameters fitted via solar-proxy cross-correlation is validated on PAMELA, AMS-02, and ACE data for long-term GCR forecasting.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10512","ref_index":24,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Turbulent Diffusion of Magnetic Field Lines in the Heliosphere","primary_cat":"astro-ph.SR","submitted_at":"2026-06-09T07:38:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02445","ref_index":280,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Counterintuitive Magnetic Connectivity and Energetic Particle Flux Differences among Nearby Spacecraft During the 2023 February 24 Solar Energetic Particle Event","primary_cat":"physics.space-ph","submitted_at":"2026-06-01T16:16:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.24143","ref_index":20,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Pitch-Angle Scattering of Cosmic Rays: Confronting Theory with Observations","primary_cat":"astro-ph.HE","submitted_at":"2026-05-22T19:05:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Observed CR pitch-angle diffusion matches quasi-slab fast-mode turbulence predictions shaped by damping, but not Alfvénic turbulence, evidencing fast-mode dominance and constraining LISM to low beta ≈0.1 with δB/B0 ≈0.5.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.23756","ref_index":26,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Probing Solar Wind Structures with Solar Energetic Particle Observations from Solar Orbiter","primary_cat":"astro-ph.SR","submitted_at":"2026-05-22T15:28:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Solar Orbiter data reveals SEP flux deflections associated with magnetic flux tubes, positioning SEPs as a diagnostic for solar wind structures.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.22729","ref_index":36,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Polarized 3D Synthetic Turbulence I: Magnetic Field Line Random Walk","primary_cat":"astro-ph.HE","submitted_at":"2026-05-21T17:01:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Magnetosonic polarization in synthetic turbulence produces field-line diffusion scaling as (δB/B)^4 with subdiffusion matching MHD simulations, unlike the (δB/B)^2 scaling for random polarization.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.03380","ref_index":34,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Data-Constrained Modeling of Electron Transport and Asymmetric Precipitation in the 2011 August 4 Solar Flare","primary_cat":"astro-ph.SR","submitted_at":"2026-05-05T05:41:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Data-constrained 3D modeling of the 2011 August 4 flare reveals strong polarity asymmetry in electron precipitation driven by magnetic mirror ratios, with turbulent scattering and Coulomb collisions modulating the energy-dependent flux.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"injected lies closer to the positive polarity (P1), which may also cause more particles to precipitate toward it. When turbulent pitch-angle scattering is present, the electron precipitation fraction shows a marked energy depen- dence, increasing with electron energy. This behavior can be understood in terms of the particle mean free path,λ ∥ = 3κ∥/v∝v 1/3, whereκ ∥ is the parallel diffusion coefficient and related toD t µµ (J. R. Jokipii 1966; X. Kong et al. 2022a; F. Yu et al. 2022). Thus, high-energy electrons have a larger mean free path and precipitate more efficiently onto the solar surface. Furthermore, the precipitation fraction exhibits a \"rise-then-fall\" trend with increasing scattering strength. As shown in Figure 5(a), for the positive polarity, the precipitation fraction in the weak scattering regime"},{"citing_arxiv_id":"2512.11062","ref_index":30,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Effects of Varied Cosmic Ray Feedback from AGN on Massive Galaxy Properties","primary_cat":"astro-ph.GA","submitted_at":"2025-12-11T19:23:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Varied cosmic ray feedback models from AGN in FIRE-3 simulations all quench massive galaxies consistently with observations but produce vastly different circumgalactic medium properties.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.07104","ref_index":136,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Cosmic Rays on Galaxy Scales: Progress and Pitfalls for CR-MHD Dynamical Models","primary_cat":"astro-ph.GA","submitted_at":"2025-09-08T18:00:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"A review summarizing pitfalls in older CR-MHD models and progress toward more rigorous treatments that connect microphysical CR scales to galactic dynamics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}