{"paper":{"title":"Magnetohydrodynamics using path or stream functions","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.EP","astro-ph.HE","physics.flu-dyn","physics.plasm-ph"],"primary_cat":"astro-ph.GA","authors_text":"Uri Keshet, Yossi Naor","submitted_at":"2015-01-27T20:12:46Z","abstract_excerpt":"Magnetization in highly conductive plasmas is ubiquitous to astronomical systems. Flows in such media can be described by three path functions $\\Lambda_\\alpha$, or, for a steady flow, by two stream functions $\\lambda_\\kappa$ and an additional field such as the mass density $\\rho$, velocity $v$, or travel time $\\Delta t$. While typical analyses of a frozen magnetic field $\\boldsymbol{B}$ are problem-specific and involve nonlocal gradients of the fluid element position $\\boldsymbol{x}(t)$, we derive the general, local (in $\\Lambda$ or $\\lambda$ space) solution $\\boldsymbol{B}=(\\partial\\boldsymbo"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1501.06892","kind":"arxiv","version":4},"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"}