{"record":{"author":{"account_ref":null,"orcid":null},"builds_on":[],"content_schema":"pubphys.content.revision/1","content_sha256":"f5455f5df7c00f2b60a7ff05aa5b9ed226fa97b7b877ec9dbf511a246c2eeb4e","created":"2026-10-03T07:17:55Z","files":[],"origin":{"assisted_by":[],"kind":"seed"},"parents":["5475cf5dc5b1a72283d26dc95dc6e00d7ea4e00096a7c6492e409a1816eeb011"],"salt":"8fb810c1de533374fbb3bdf78c98bcf6f9b068e073fae777d10b5e4742cbd292","schema":"pubphys.record/2","site":"pubphys.com","target":null,"type":"revision"},"content":{"answer_type":"identification","assisted_by":[],"external_id":"astro.pulsars-magnetars.magnetar-field-origin","kind":"phenomenon","literature_status":"contested","n":"1","parents":[],"plain":"The field could be inherited from a strongly magnetic parent star or amplified by a dynamo (stirring motions that regenerate magnetic field) during the collapse.","posed_since":"1992","precise":"Determine whether magnetar dipole fields $B \\sim 1e14\\ \\text{to}\\ 1e15\\ \\mathrm{G}$ arise from flux conservation of fossil fields in magnetic massive stars (possibly stellar-merger products), from convective or magnetorotational dynamos in a proto-neutron star spinning at $P$ of a few ms, or from a fall-back-driven Tayler-Spruit dynamo. Answer: the channel or channels consistent with the magnetar birth fraction (estimates ~10 to 40 percent of neutron stars), ordinary supernova remnant energies and kick distributions.","problem_ref":null,"references":"","settled_by":"Proto-neutron star dynamo simulations predicting field strengths and topology, compared with magnetar population statistics and remnant energetics.","status_note":"","title":"How do magnetars acquire fields of $1\\mathrm{e}14\\ \\text{to}\\ 1\\mathrm{e}15\\,\\mathrm{G}$?","topic_ref":"cf74b0d6cbf0f14a95f95d071c68e45a587fcae015fdd13da4686d4a258fa561"},"attested":{"attestation":{"batch":null,"client_id":null,"id_token_sha256":null,"kind":"platform"},"record_hash":"9eb0d15c003029e824ce85bb558f52009c201f759cf9296f98440c8d005caa35","schema":"pubphys.attested/1"},"envelope":{"attested_hash":"c1c9c2a63b96e50a644d29802221bf1f8205e610b8a2b709c74e0ac3c7c02569","platform_signature":{"key_id":"c6afc19b31429869751f06879c75cd64ea92654423d15b44be775bf1310a60da","sig":"DSbC5zrlJaOw2Y_5kRPv2rCRW85sXJHg5Fysz9fOT2DP1khtNnU4GaPv5T_9BPHI2u0ZmvTsqjJetwvjRwx3Dg"},"schema":"pubphys.envelope/1"},"record_hash":"9eb0d15c003029e824ce85bb558f52009c201f759cf9296f98440c8d005caa35","leaf_index":587}