{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:3PWZFFPFMVCYBLAKI6OKIE6MIQ","short_pith_number":"pith:3PWZFFPF","schema_version":"1.0","canonical_sha256":"dbed9295e5654580ac0a479ca413cc4428e4f8065a68f6a04313d3dd6077eaf8","source":{"kind":"arxiv","id":"0905.4055","version":1},"attestation_state":"computed","paper":{"title":"The existence of relativistic stars in f(R) gravity","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Amol Upadhye, Wayne Hu","submitted_at":"2009-05-25T18:08:38Z","abstract_excerpt":"We refute recent claims in the literature that stars with relativistically deep potentials cannot exist in $f(R)$ gravity. Numerical examples of stable stars, including relativistic ($GM_\\star/r_\\star \\sim 0.1$), constant density stars, are studied. As a star is made larger, non-linear \"chameleon\" effects screen much of the star's mass, stabilizing gravity at the stellar center. Furthermore, we show that the onset of this chameleon screening is unrelated to strong gravity. At large central pressures $P>\\rho/3$, $f(R)$ gravity, like general relativity, does have a maximum gravitational potentia"},"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":"0905.4055","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2009-05-25T18:08:38Z","cross_cats_sorted":["astro-ph.SR","hep-ph"],"title_canon_sha256":"7d8804147f177fa684187ca1ba68109c606e9d5d3b0dcf3b6de3ec550af4c1a8","abstract_canon_sha256":"47e0df643f5b138c38381a7504944ce2a31393e384eb0a50bbfae94359fa10c5"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:21:49.975211Z","signature_b64":"adMDFEzfW1l3xORA+azfQxgO4B7FbdGCe+Mq4c/tYOONaZRuGaJH8K0f+9NUEG946etAC/lcSJJu2VZO3iChBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"dbed9295e5654580ac0a479ca413cc4428e4f8065a68f6a04313d3dd6077eaf8","last_reissued_at":"2026-07-04T16:21:49.974825Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:21:49.974825Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The existence of relativistic stars in f(R) gravity","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Amol Upadhye, Wayne Hu","submitted_at":"2009-05-25T18:08:38Z","abstract_excerpt":"We refute recent claims in the literature that stars with relativistically deep potentials cannot exist in $f(R)$ gravity. Numerical examples of stable stars, including relativistic ($GM_\\star/r_\\star \\sim 0.1$), constant density stars, are studied. As a star is made larger, non-linear \"chameleon\" effects screen much of the star's mass, stabilizing gravity at the stellar center. Furthermore, we show that the onset of this chameleon screening is unrelated to strong gravity. At large central pressures $P>\\rho/3$, $f(R)$ gravity, like general relativity, does have a maximum gravitational potentia"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0905.4055","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/0905.4055/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":"0905.4055","created_at":"2026-07-04T16:21:49.974886+00:00"},{"alias_kind":"arxiv_version","alias_value":"0905.4055v1","created_at":"2026-07-04T16:21:49.974886+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0905.4055","created_at":"2026-07-04T16:21:49.974886+00:00"},{"alias_kind":"pith_short_12","alias_value":"3PWZFFPFMVCY","created_at":"2026-07-04T16:21:49.974886+00:00"},{"alias_kind":"pith_short_16","alias_value":"3PWZFFPFMVCYBLAK","created_at":"2026-07-04T16:21:49.974886+00:00"},{"alias_kind":"pith_short_8","alias_value":"3PWZFFPF","created_at":"2026-07-04T16:21:49.974886+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"1501.07274","citing_title":"Testing General Relativity with Present and Future Astrophysical Observations","ref_index":147,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/3PWZFFPFMVCYBLAKI6OKIE6MIQ","json":"https://pith.science/pith/3PWZFFPFMVCYBLAKI6OKIE6MIQ.json","graph_json":"https://pith.science/api/pith-number/3PWZFFPFMVCYBLAKI6OKIE6MIQ/graph.json","events_json":"https://pith.science/api/pith-number/3PWZFFPFMVCYBLAKI6OKIE6MIQ/events.json","paper":"https://pith.science/paper/3PWZFFPF"},"agent_actions":{"view_html":"https://pith.science/pith/3PWZFFPFMVCYBLAKI6OKIE6MIQ","download_json":"https://pith.science/pith/3PWZFFPFMVCYBLAKI6OKIE6MIQ.json","view_paper":"https://pith.science/paper/3PWZFFPF","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0905.4055&json=true","fetch_graph":"https://pith.science/api/pith-number/3PWZFFPFMVCYBLAKI6OKIE6MIQ/graph.json","fetch_events":"https://pith.science/api/pith-number/3PWZFFPFMVCYBLAKI6OKIE6MIQ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/3PWZFFPFMVCYBLAKI6OKIE6MIQ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/3PWZFFPFMVCYBLAKI6OKIE6MIQ/action/storage_attestation","attest_author":"https://pith.science/pith/3PWZFFPFMVCYBLAKI6OKIE6MIQ/action/author_attestation","sign_citation":"https://pith.science/pith/3PWZFFPFMVCYBLAKI6OKIE6MIQ/action/citation_signature","submit_replication":"https://pith.science/pith/3PWZFFPFMVCYBLAKI6OKIE6MIQ/action/replication_record"}},"created_at":"2026-07-04T16:21:49.974886+00:00","updated_at":"2026-07-04T16:21:49.974886+00:00"}