{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:K74X2RAAEP7MHBER7PQ5QHB7BM","short_pith_number":"pith:K74X2RAA","schema_version":"1.0","canonical_sha256":"57f97d440023fec38491fbe1d81c3f0b3d85ca2307e27c6f391fe8cc04cce81c","source":{"kind":"arxiv","id":"1706.04630","version":2},"attestation_state":"computed","paper":{"title":"Muon Creation in Supernova Matter Facilitates Neutrino-driven Explosions","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ph","nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"2), (2) Physik Dept., (3) GSI Darmstadt, 4), (4) TU Darmstadt, (5) Indiana Univ., A. Lohs (3), Bloomington), C.J. Horowitz (5), Garching, G. Martinez-Pinedo (3, H.-Th. Janka (2), R. Bollig (1, T. Melson (1) ((1) MPI Astrophysics, TUM","submitted_at":"2017-06-14T18:34:23Z","abstract_excerpt":"Muons can be created in nascent neutron stars (NSs) due to the high electron chemical potentials and the high temperatures. Because of their relatively lower abundance compared to electrons, their role has so far been ignored in numerical simulations of stellar core collapse and NS formation. However, the appearance of muons softens the NS equation of state, triggers faster NS contraction and thus leads to higher luminosities and mean energies of the emitted neutrinos. This strengthens the postshock heating by neutrinos and can facilitate explosions by the neutrino-driven mechanism."},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"1706.04630","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2017-06-14T18:34:23Z","cross_cats_sorted":["hep-ph","nucl-th"],"title_canon_sha256":"43ee4e4794dccc0ececb6db858dad5b70bea9aed5162f2f95d01450dec83167b","abstract_canon_sha256":"139a3e44fdcb5044d6581a87062898ae068dba9a3267e324b04c93ebe84f3c40"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:27:46.432254Z","signature_b64":"4j95LoXkC2AY1M0T8omqrLQkIs+MHg8P+sS/q/XGf4QJCFQ5PNH898Qr8++OBFFlqQO++uImNx/Yt02pfeTODg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"57f97d440023fec38491fbe1d81c3f0b3d85ca2307e27c6f391fe8cc04cce81c","last_reissued_at":"2026-05-18T00:27:46.431731Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:27:46.431731Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Muon Creation in Supernova Matter Facilitates Neutrino-driven Explosions","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ph","nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"2), (2) Physik Dept., (3) GSI Darmstadt, 4), (4) TU Darmstadt, (5) Indiana Univ., A. Lohs (3), Bloomington), C.J. Horowitz (5), Garching, G. Martinez-Pinedo (3, H.-Th. Janka (2), R. Bollig (1, T. Melson (1) ((1) MPI Astrophysics, TUM","submitted_at":"2017-06-14T18:34:23Z","abstract_excerpt":"Muons can be created in nascent neutron stars (NSs) due to the high electron chemical potentials and the high temperatures. Because of their relatively lower abundance compared to electrons, their role has so far been ignored in numerical simulations of stellar core collapse and NS formation. However, the appearance of muons softens the NS equation of state, triggers faster NS contraction and thus leads to higher luminosities and mean energies of the emitted neutrinos. This strengthens the postshock heating by neutrinos and can facilitate explosions by the neutrino-driven mechanism."},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1706.04630","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"},"aliases":[{"alias_kind":"arxiv","alias_value":"1706.04630","created_at":"2026-05-18T00:27:46.431816+00:00"},{"alias_kind":"arxiv_version","alias_value":"1706.04630v2","created_at":"2026-05-18T00:27:46.431816+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1706.04630","created_at":"2026-05-18T00:27:46.431816+00:00"},{"alias_kind":"pith_short_12","alias_value":"K74X2RAAEP7M","created_at":"2026-05-18T12:31:24.725408+00:00"},{"alias_kind":"pith_short_16","alias_value":"K74X2RAAEP7MHBER","created_at":"2026-05-18T12:31:24.725408+00:00"},{"alias_kind":"pith_short_8","alias_value":"K74X2RAA","created_at":"2026-05-18T12:31:24.725408+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":7,"internal_anchor_count":6,"sample":[{"citing_arxiv_id":"2109.03244","citing_title":"Muonic Boson Limits: Supernova Redux","ref_index":8,"is_internal_anchor":true},{"citing_arxiv_id":"2511.09619","citing_title":"$L_\\mu-L_\\tau$ gauge bosons in beam dumps and supernovae","ref_index":57,"is_internal_anchor":true},{"citing_arxiv_id":"2605.18972","citing_title":"Flavor Conversion Enhances or Suppresses Supernova Explodability Independent of the Progenitor Mass","ref_index":94,"is_internal_anchor":true},{"citing_arxiv_id":"2605.17563","citing_title":"Charged-current neutrino opacity within the relativistic Hartree-Fock framework for astrophysical simulations of core-collapse supernovae and binary neutron star mergers","ref_index":63,"is_internal_anchor":true},{"citing_arxiv_id":"2509.13322","citing_title":"Axion-photon conversion in transient compact stars: Systematics, constraints, and opportunities","ref_index":62,"is_internal_anchor":true},{"citing_arxiv_id":"2601.11272","citing_title":"Intermittent Turbulence, Fast Flavor Conversion, and Observable Supernova Probes","ref_index":3,"is_internal_anchor":true},{"citing_arxiv_id":"2604.01277","citing_title":"Lights, Camera, Axion: Tracing Axions from Supernovae in the Diffuse $\\gamma$-ray Sky","ref_index":87,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/K74X2RAAEP7MHBER7PQ5QHB7BM","json":"https://pith.science/pith/K74X2RAAEP7MHBER7PQ5QHB7BM.json","graph_json":"https://pith.science/api/pith-number/K74X2RAAEP7MHBER7PQ5QHB7BM/graph.json","events_json":"https://pith.science/api/pith-number/K74X2RAAEP7MHBER7PQ5QHB7BM/events.json","paper":"https://pith.science/paper/K74X2RAA"},"agent_actions":{"view_html":"https://pith.science/pith/K74X2RAAEP7MHBER7PQ5QHB7BM","download_json":"https://pith.science/pith/K74X2RAAEP7MHBER7PQ5QHB7BM.json","view_paper":"https://pith.science/paper/K74X2RAA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1706.04630&json=true","fetch_graph":"https://pith.science/api/pith-number/K74X2RAAEP7MHBER7PQ5QHB7BM/graph.json","fetch_events":"https://pith.science/api/pith-number/K74X2RAAEP7MHBER7PQ5QHB7BM/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/K74X2RAAEP7MHBER7PQ5QHB7BM/action/timestamp_anchor","attest_storage":"https://pith.science/pith/K74X2RAAEP7MHBER7PQ5QHB7BM/action/storage_attestation","attest_author":"https://pith.science/pith/K74X2RAAEP7MHBER7PQ5QHB7BM/action/author_attestation","sign_citation":"https://pith.science/pith/K74X2RAAEP7MHBER7PQ5QHB7BM/action/citation_signature","submit_replication":"https://pith.science/pith/K74X2RAAEP7MHBER7PQ5QHB7BM/action/replication_record"}},"created_at":"2026-05-18T00:27:46.431816+00:00","updated_at":"2026-05-18T00:27:46.431816+00:00"}