{"paper":{"title":"Electron heat conduction in the solar wind: transition from Spitzer-H\\\"{a}rm to the collisionless limit","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["physics.plasm-ph","physics.space-ph"],"primary_cat":"astro-ph.SR","authors_text":"C. H. K. Chen, C. Salem, E. Quataert, M. Pulupa, S. D. Bale","submitted_at":"2013-03-05T05:51:40Z","abstract_excerpt":"We use a statistically significant set of measurements to show that the field-aligned electron heat flux $q_\\parallel$ in the solar wind at 1 AU is consistent with the Spitzer-H\\\"{a}rm collisional heat flux $q_{sh}$ for temperature gradient scales larger than a few mean free paths $L_T \\gtrsim 3.5 ~\\lambda_{fp}$. This represents about 65% of the measured data and corresponds primarily to high $\\beta$, weakly collisional plasma ('slow solar wind'). In the more collisionless regime $\\lambda_{fp}/L_T \\gtrsim 0.28$, the electron heat flux is limited to $q_\\parallel/q_0 \\sim 0.3$, independent of me"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1303.0932","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"}