{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:73KO3MWJJ7WIYTCG3SEKPBVFOA","short_pith_number":"pith:73KO3MWJ","schema_version":"1.0","canonical_sha256":"fed4edb2c94fec8c4c46dc88a786a57026292fd831bbdd432386720e788db584","source":{"kind":"arxiv","id":"1307.1436","version":1},"attestation_state":"computed","paper":{"title":"Imprint of the symmetry energy on the inner crust and strangeness content of neutron stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"nucl-th","authors_text":"Aziz Rabhi, Camille Ducoin, Constan\\c{c}a Provid\\^encia, D\\'ebora P. Menezes, Fabrizio Grill, Isaac Vida\\~na, J\\'er\\^ome Margueron, Rafael Cavagnoli, Sidney S. Avancini, Silvia Chiacchiera","submitted_at":"2013-07-04T18:07:45Z","abstract_excerpt":"In this work we study the effect of the symmetry energy on several properties of neutron stars. First, we discuss its effect on the density, proton fraction and pressure of the neutron star crust-core transition. We show that whereas the first two quantities present a clear correlation with the slope parameter $L$ of the symmetry energy, no satisfactory correlation is seen between the transition pressure and $L$. However, a linear combination of the slope and curvature parameters at $\\rho=0.1$ fm$^{-3}$ is well correlated with the transition pressure. In the second part we analyze the effect o"},"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":"1307.1436","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"nucl-th","submitted_at":"2013-07-04T18:07:45Z","cross_cats_sorted":[],"title_canon_sha256":"1ddf426ab2358128dccbd0b9293d7339ba292674948674ab0c955ce241aa65c1","abstract_canon_sha256":"c3252933dffff553e498e21bc6238f6078b4a7b817ddf2eadd5d72718c6380c8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:48:59.634268Z","signature_b64":"RhOAswhxm2G6MGctYYOIqLBQZNYvN8iPP8GI511pc7w3ZwDmoOSw4oiy6EK416/wK3TbGAHIHNqkR3vyp3TEAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"fed4edb2c94fec8c4c46dc88a786a57026292fd831bbdd432386720e788db584","last_reissued_at":"2026-05-18T01:48:59.633819Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:48:59.633819Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Imprint of the symmetry energy on the inner crust and strangeness content of neutron stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"nucl-th","authors_text":"Aziz Rabhi, Camille Ducoin, Constan\\c{c}a Provid\\^encia, D\\'ebora P. Menezes, Fabrizio Grill, Isaac Vida\\~na, J\\'er\\^ome Margueron, Rafael Cavagnoli, Sidney S. Avancini, Silvia Chiacchiera","submitted_at":"2013-07-04T18:07:45Z","abstract_excerpt":"In this work we study the effect of the symmetry energy on several properties of neutron stars. First, we discuss its effect on the density, proton fraction and pressure of the neutron star crust-core transition. We show that whereas the first two quantities present a clear correlation with the slope parameter $L$ of the symmetry energy, no satisfactory correlation is seen between the transition pressure and $L$. However, a linear combination of the slope and curvature parameters at $\\rho=0.1$ fm$^{-3}$ is well correlated with the transition pressure. In the second part we analyze the effect o"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1307.1436","kind":"arxiv","version":1},"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":"1307.1436","created_at":"2026-05-18T01:48:59.633882+00:00"},{"alias_kind":"arxiv_version","alias_value":"1307.1436v1","created_at":"2026-05-18T01:48:59.633882+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1307.1436","created_at":"2026-05-18T01:48:59.633882+00:00"},{"alias_kind":"pith_short_12","alias_value":"73KO3MWJJ7WI","created_at":"2026-05-18T12:27:36.564083+00:00"},{"alias_kind":"pith_short_16","alias_value":"73KO3MWJJ7WIYTCG","created_at":"2026-05-18T12:27:36.564083+00:00"},{"alias_kind":"pith_short_8","alias_value":"73KO3MWJ","created_at":"2026-05-18T12:27:36.564083+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2504.18764","citing_title":"Symmetry Energy Expansion with Strange Dense Matter","ref_index":73,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/73KO3MWJJ7WIYTCG3SEKPBVFOA","json":"https://pith.science/pith/73KO3MWJJ7WIYTCG3SEKPBVFOA.json","graph_json":"https://pith.science/api/pith-number/73KO3MWJJ7WIYTCG3SEKPBVFOA/graph.json","events_json":"https://pith.science/api/pith-number/73KO3MWJJ7WIYTCG3SEKPBVFOA/events.json","paper":"https://pith.science/paper/73KO3MWJ"},"agent_actions":{"view_html":"https://pith.science/pith/73KO3MWJJ7WIYTCG3SEKPBVFOA","download_json":"https://pith.science/pith/73KO3MWJJ7WIYTCG3SEKPBVFOA.json","view_paper":"https://pith.science/paper/73KO3MWJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1307.1436&json=true","fetch_graph":"https://pith.science/api/pith-number/73KO3MWJJ7WIYTCG3SEKPBVFOA/graph.json","fetch_events":"https://pith.science/api/pith-number/73KO3MWJJ7WIYTCG3SEKPBVFOA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/73KO3MWJJ7WIYTCG3SEKPBVFOA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/73KO3MWJJ7WIYTCG3SEKPBVFOA/action/storage_attestation","attest_author":"https://pith.science/pith/73KO3MWJJ7WIYTCG3SEKPBVFOA/action/author_attestation","sign_citation":"https://pith.science/pith/73KO3MWJJ7WIYTCG3SEKPBVFOA/action/citation_signature","submit_replication":"https://pith.science/pith/73KO3MWJJ7WIYTCG3SEKPBVFOA/action/replication_record"}},"created_at":"2026-05-18T01:48:59.633882+00:00","updated_at":"2026-05-18T01:48:59.633882+00:00"}