{"paper":{"title":"Collisionless Isotropization of the Solar-Wind Protons by Compressive Fluctuations and Plasma Instabilities","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR","physics.plasm-ph"],"primary_cat":"physics.space-ph","authors_text":"Benjamin D. G. Chandran (UNH), Daniel Verscharen (UNH), Eliot Quataert (UCB), Kristopher G. Klein (UNH)","submitted_at":"2016-05-23T19:17:25Z","abstract_excerpt":"Compressive fluctuations are a minor yet significant component of astrophysical plasma turbulence. In the solar wind, long-wavelength compressive slow-mode fluctuations lead to changes in $\\beta_{\\parallel \\mathrm p}\\equiv 8\\pi n_{\\mathrm p}k_{\\mathrm B}T_{\\parallel \\mathrm p}/B^2$ and in $R_{\\mathrm p}\\equiv T_{\\perp \\mathrm p}/T_{\\parallel \\mathrm p}$, where $T_{\\perp \\mathrm p}$ and $T_{\\parallel \\mathrm p}$ are the perpendicular and parallel temperatures of the protons, $B$ is the magnetic field strength, and $n_{\\mathrm p}$ is the proton density. If the amplitude of the compressive fluctu"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1605.07143","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}