{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:JZT647VUQTGHTWYEVYZNZ5IZIY","short_pith_number":"pith:JZT647VU","schema_version":"1.0","canonical_sha256":"4e67ee7eb484cc79db04ae32dcf519463478e9ec8c2e06c27f8e81ddf07ff98f","source":{"kind":"arxiv","id":"2001.08504","version":1},"attestation_state":"computed","paper":{"title":"Supermassive Neutron Stars in Axion $F(R)$ Gravity","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","hep-th"],"primary_cat":"gr-qc","authors_text":"Artyom V. Astashenok, Sergey D. Odintsov","submitted_at":"2020-01-23T13:48:59Z","abstract_excerpt":"We investigated realistic neutron stars in axion $R^{2}$ gravity. The coupling between curvature and axion field $\\phi$ is assumed in the simple form $\\sim R^2\\phi$. For the axion mass in the range $m_{a}\\sim 10^{-11}-10^{-10}$ eV the solitonic core within neutron star and corresponding halo with size $\\sim 100$ km can exist. Therefore the effective contribution of $R^2$ term grows inside the star and it leads to change of star parameters (namely, mass and radius). We obtained the increase of star mass independent from central density for wide range of masses. Therefore, maximal possible mass "},"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":"2001.08504","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2020-01-23T13:48:59Z","cross_cats_sorted":["astro-ph.HE","hep-th"],"title_canon_sha256":"60a5984248115469b3b7f35ed1e7af90d61ff8cfa49b2521b2d4e0cea3960645","abstract_canon_sha256":"687062edb87e9e4cf337bf9a0589ccd678d27c20b1022e55c57008ba3891d172"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:36:47.831278Z","signature_b64":"ivZpCmb6M3p5jVbxZLqTTcvizXmyLWSBIKN2GTDPcIU4ADLRu96S4Vx4iUbpLbKMPDYracmgkrUAW/8p+QC2Ag==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4e67ee7eb484cc79db04ae32dcf519463478e9ec8c2e06c27f8e81ddf07ff98f","last_reissued_at":"2026-07-05T00:36:47.830892Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:36:47.830892Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Supermassive Neutron Stars in Axion $F(R)$ Gravity","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","hep-th"],"primary_cat":"gr-qc","authors_text":"Artyom V. Astashenok, Sergey D. Odintsov","submitted_at":"2020-01-23T13:48:59Z","abstract_excerpt":"We investigated realistic neutron stars in axion $R^{2}$ gravity. The coupling between curvature and axion field $\\phi$ is assumed in the simple form $\\sim R^2\\phi$. For the axion mass in the range $m_{a}\\sim 10^{-11}-10^{-10}$ eV the solitonic core within neutron star and corresponding halo with size $\\sim 100$ km can exist. Therefore the effective contribution of $R^2$ term grows inside the star and it leads to change of star parameters (namely, mass and radius). We obtained the increase of star mass independent from central density for wide range of masses. Therefore, maximal possible mass "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2001.08504","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2001.08504/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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":"2001.08504","created_at":"2026-07-05T00:36:47.830956+00:00"},{"alias_kind":"arxiv_version","alias_value":"2001.08504v1","created_at":"2026-07-05T00:36:47.830956+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2001.08504","created_at":"2026-07-05T00:36:47.830956+00:00"},{"alias_kind":"pith_short_12","alias_value":"JZT647VUQTGH","created_at":"2026-07-05T00:36:47.830956+00:00"},{"alias_kind":"pith_short_16","alias_value":"JZT647VUQTGHTWYE","created_at":"2026-07-05T00:36:47.830956+00:00"},{"alias_kind":"pith_short_8","alias_value":"JZT647VU","created_at":"2026-07-05T00:36:47.830956+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2412.03219","citing_title":"Neutron star in Logarithmic model of Cartan $F(R)$ gravity","ref_index":14,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/JZT647VUQTGHTWYEVYZNZ5IZIY","json":"https://pith.science/pith/JZT647VUQTGHTWYEVYZNZ5IZIY.json","graph_json":"https://pith.science/api/pith-number/JZT647VUQTGHTWYEVYZNZ5IZIY/graph.json","events_json":"https://pith.science/api/pith-number/JZT647VUQTGHTWYEVYZNZ5IZIY/events.json","paper":"https://pith.science/paper/JZT647VU"},"agent_actions":{"view_html":"https://pith.science/pith/JZT647VUQTGHTWYEVYZNZ5IZIY","download_json":"https://pith.science/pith/JZT647VUQTGHTWYEVYZNZ5IZIY.json","view_paper":"https://pith.science/paper/JZT647VU","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2001.08504&json=true","fetch_graph":"https://pith.science/api/pith-number/JZT647VUQTGHTWYEVYZNZ5IZIY/graph.json","fetch_events":"https://pith.science/api/pith-number/JZT647VUQTGHTWYEVYZNZ5IZIY/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/JZT647VUQTGHTWYEVYZNZ5IZIY/action/timestamp_anchor","attest_storage":"https://pith.science/pith/JZT647VUQTGHTWYEVYZNZ5IZIY/action/storage_attestation","attest_author":"https://pith.science/pith/JZT647VUQTGHTWYEVYZNZ5IZIY/action/author_attestation","sign_citation":"https://pith.science/pith/JZT647VUQTGHTWYEVYZNZ5IZIY/action/citation_signature","submit_replication":"https://pith.science/pith/JZT647VUQTGHTWYEVYZNZ5IZIY/action/replication_record"}},"created_at":"2026-07-05T00:36:47.830956+00:00","updated_at":"2026-07-05T00:36:47.830956+00:00"}