{"paper":{"title":"Magnetic field alignment with dense cores in the transition between cloud and core scales","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"Magnetic fields lose coherent alignment when moving from cloud scales to dense core scales in star-forming regions.","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"Ayush Pandhi, Doug Johnstone, Fr\\'ed\\'erick Poidevin, James Di Francesco, Laura Fissel, Mehrnoosh Tahani, Rachel Friesen, Sarah Sadavoy, Sean Yin, Simon Coud\\'e","submitted_at":"2026-04-10T18:00:13Z","abstract_excerpt":"In a magnetically-dominated model of star formation, we expect to see alignments between the magnetic field orientation of star-forming dense cores and the cloud-scale magnetic field. Pandhi et al. (2023) showed instead, however, that the orientation of cores and their angular momentum vectors appear random with respect to the larger-scale magnetic field, implying that magnetic fields may play a diminished role in core formation and evolution. Here, we use higher-resolution dust polarization data from the B-Fields In Star-forming Region Observations (BISTRO) survey on the James Clerk Maxwell T"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"We conclude that there is a clear change in the magnetic field in the transition from cloud- to core-scales. Our results suggest that the magnetic field may not play a dominant role in the evolution of dense cores on core scales.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"That the observed dust polarization reliably traces the plane-of-sky magnetic field orientation at both cloud and core scales without significant contamination from other effects such as grain alignment efficiency changes or line-of-sight confusion.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Core-scale magnetic fields in star-forming regions are more disordered than cloud-scale fields and align randomly with core orientations and velocity gradients.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Magnetic fields lose coherent alignment when moving from cloud scales to dense core scales in star-forming regions.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"e3eb40eb4794fa5686ae0670354b4ad11497432590e690db825f9d1dcf553ae5"},"source":{"id":"2604.09770","kind":"arxiv","version":1},"verdict":{"id":"28482dc3-0d94-495e-b709-c4730697135d","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-10T16:27:58.885453Z","strongest_claim":"We conclude that there is a clear change in the magnetic field in the transition from cloud- to core-scales. Our results suggest that the magnetic field may not play a dominant role in the evolution of dense cores on core scales.","one_line_summary":"Core-scale magnetic fields in star-forming regions are more disordered than cloud-scale fields and align randomly with core orientations and velocity gradients.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"That the observed dust polarization reliably traces the plane-of-sky magnetic field orientation at both cloud and core scales without significant contamination from other effects such as grain alignment efficiency changes or line-of-sight confusion.","pith_extraction_headline":"Magnetic fields lose coherent alignment when moving from cloud scales to dense core scales in star-forming regions."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2604.09770/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":81,"sample":[{"doi":"10.48550/arxiv.2501.13931","year":2025,"title":"2025, arXiv e-prints, arXiv:2501.13931, 10.48550/arXiv.2501.13931","work_id":"cf4832a2-2ad3-4199-8cea-88a4845900f1","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1080/01621459.1954.10501232","year":1954,"title":"W., & Darling, D","work_id":"9ceb9c99-588c-4292-8e93-b42a0215b37d","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1146/annurev-astro-082214-122414","year":2015,"title":", year = 2015, month = aug, volume =","work_id":"bc3270ee-6534-4a27-863b-9e68ce1621ec","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1051/0004-6361/201014666","year":2010,"title":"2010, , 518, L102, 10.1051/0004-6361/201014666","work_id":"c3d4009e-63ab-4b0b-8782-0d302acb611f","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1051/0004-6361/202038024","year":2020,"title":"Arce-Tord , C., Louvet , F., Cortes , P. C., et al. 2020, , 640, A111, 10.1051/0004-6361/202038024","work_id":"96d2f59e-7050-4dd5-9b2c-4a7f536a2ee3","ref_index":5,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":81,"snapshot_sha256":"37a22ead9216406be1173bc388d1ecbbacf7f88b91f5354398beed146aec2815","internal_anchors":1},"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"}