{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2010:ZY2NAQNGHG4MF6EVGXJSTHF7PZ","short_pith_number":"pith:ZY2NAQNG","schema_version":"1.0","canonical_sha256":"ce34d041a639b8c2f89535d3299cbf7e5921820dfc5b23d12afcd56b8a27a50b","source":{"kind":"arxiv","id":"1101.0219","version":1},"attestation_state":"computed","paper":{"title":"Hydrostatic equilibrium and stellar structure in 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":"A. Stabile, M. De Laurentis, S. Capozziello, S.D. Odintsov","submitted_at":"2010-12-31T08:45:39Z","abstract_excerpt":"We investigate the hydrostatic equilibrium of stellar structure by taking into account the modi- fied La\\'e-Emden equation coming out from f(R)-gravity. Such an equation is obtained in metric approach by considering the Newtonian limit of f(R)-gravity, which gives rise to a modified Poisson equation, and then introducing a relation between pressure and density with polytropic index n. The modified equation results an integro-differential equation, which, in the limit f(R) \\rightarrow R, becomes the standard La\\'e-Emden equation. We find the radial profiles of gravitational potential by solving"},"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":"1101.0219","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2010-12-31T08:45:39Z","cross_cats_sorted":["astro-ph.HE","hep-th"],"title_canon_sha256":"47c1735dd33d319cee36684840992ed2f97fbc45c989c0575740615206a74d1b","abstract_canon_sha256":"4c515e316fa39ec257d273a42ac33aa45283126d8cb786c8a00037127d04655e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:26:32.681597Z","signature_b64":"jUG1JnT/zwPTGm7qGv80h+Pj2QWclghcyD/ZtNQid7wg8XUAvNKlArvkARXRBfE9AV9wM7LZU8XM8v+vrY5CAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ce34d041a639b8c2f89535d3299cbf7e5921820dfc5b23d12afcd56b8a27a50b","last_reissued_at":"2026-05-18T04:26:32.681009Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:26:32.681009Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Hydrostatic equilibrium and stellar structure in 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":"A. Stabile, M. De Laurentis, S. Capozziello, S.D. Odintsov","submitted_at":"2010-12-31T08:45:39Z","abstract_excerpt":"We investigate the hydrostatic equilibrium of stellar structure by taking into account the modi- fied La\\'e-Emden equation coming out from f(R)-gravity. Such an equation is obtained in metric approach by considering the Newtonian limit of f(R)-gravity, which gives rise to a modified Poisson equation, and then introducing a relation between pressure and density with polytropic index n. The modified equation results an integro-differential equation, which, in the limit f(R) \\rightarrow R, becomes the standard La\\'e-Emden equation. We find the radial profiles of gravitational potential by solving"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1101.0219","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":"1101.0219","created_at":"2026-05-18T04:26:32.681087+00:00"},{"alias_kind":"arxiv_version","alias_value":"1101.0219v1","created_at":"2026-05-18T04:26:32.681087+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1101.0219","created_at":"2026-05-18T04:26:32.681087+00:00"},{"alias_kind":"pith_short_12","alias_value":"ZY2NAQNGHG4M","created_at":"2026-05-18T12:26:18.847500+00:00"},{"alias_kind":"pith_short_16","alias_value":"ZY2NAQNGHG4MF6EV","created_at":"2026-05-18T12:26:18.847500+00:00"},{"alias_kind":"pith_short_8","alias_value":"ZY2NAQNG","created_at":"2026-05-18T12:26:18.847500+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.13011","citing_title":"Buchdahl Limit and TOV Equations in Interacting Vacuum Scenarios","ref_index":11,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ZY2NAQNGHG4MF6EVGXJSTHF7PZ","json":"https://pith.science/pith/ZY2NAQNGHG4MF6EVGXJSTHF7PZ.json","graph_json":"https://pith.science/api/pith-number/ZY2NAQNGHG4MF6EVGXJSTHF7PZ/graph.json","events_json":"https://pith.science/api/pith-number/ZY2NAQNGHG4MF6EVGXJSTHF7PZ/events.json","paper":"https://pith.science/paper/ZY2NAQNG"},"agent_actions":{"view_html":"https://pith.science/pith/ZY2NAQNGHG4MF6EVGXJSTHF7PZ","download_json":"https://pith.science/pith/ZY2NAQNGHG4MF6EVGXJSTHF7PZ.json","view_paper":"https://pith.science/paper/ZY2NAQNG","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1101.0219&json=true","fetch_graph":"https://pith.science/api/pith-number/ZY2NAQNGHG4MF6EVGXJSTHF7PZ/graph.json","fetch_events":"https://pith.science/api/pith-number/ZY2NAQNGHG4MF6EVGXJSTHF7PZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ZY2NAQNGHG4MF6EVGXJSTHF7PZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ZY2NAQNGHG4MF6EVGXJSTHF7PZ/action/storage_attestation","attest_author":"https://pith.science/pith/ZY2NAQNGHG4MF6EVGXJSTHF7PZ/action/author_attestation","sign_citation":"https://pith.science/pith/ZY2NAQNGHG4MF6EVGXJSTHF7PZ/action/citation_signature","submit_replication":"https://pith.science/pith/ZY2NAQNGHG4MF6EVGXJSTHF7PZ/action/replication_record"}},"created_at":"2026-05-18T04:26:32.681087+00:00","updated_at":"2026-05-18T04:26:32.681087+00:00"}