{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2002:LWYLH3C3DZMEKJCGCBSDHGSGHH","short_pith_number":"pith:LWYLH3C3","schema_version":"1.0","canonical_sha256":"5db0b3ec5b1e584524461064339a4639fffca854688d3a23b2c73c5e78b6cf3e","source":{"kind":"arxiv","id":"astro-ph/0212186","version":1},"attestation_state":"computed","paper":{"title":"Stability of accretion disk around rotating black holes: a pseudo-general-relativistic fluid dynamical study","license":"","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph","authors_text":"Banibrata Mukhopadhyay","submitted_at":"2002-12-07T19:00:11Z","abstract_excerpt":"We discuss the solution of accretion disk when the black hole is chosen to be rotating. We study, how the fluid properties get affected for different rotation parameters of the black hole. We know that no cosmic object is static in Universe. Here the effect of the rotation of the black hole to the space-time is considered following an earlier work of the author, where the pseudo-Newtonian potential was prescribed for the Kerr geometry. We show that, with the inclusion of rotation of the black hole, the valid disk parameter region dramatically changes and disk becomes unstable. Also we discuss "},"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":"astro-ph/0212186","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2002-12-07T19:00:11Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"2b6f2b7b413eb08e40fc2480a82cbcf9375d439e36abb7c815e3e01ac6d70534","abstract_canon_sha256":"439a22c2e53c8620074a6890d3a99eb727b426d717af2908cf5da827066a22df"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:31:22.621013Z","signature_b64":"TS0DL8A3giGMAXA/Mk8KM3ZYdRaSoUbxdblEzbt39oDZP8lp0m5Syb1A1/1GImRlbk1vRzTH3FyOnQ5e+l/iCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"5db0b3ec5b1e584524461064339a4639fffca854688d3a23b2c73c5e78b6cf3e","last_reissued_at":"2026-07-04T16:31:22.620581Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:31:22.620581Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Stability of accretion disk around rotating black holes: a pseudo-general-relativistic fluid dynamical study","license":"","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph","authors_text":"Banibrata Mukhopadhyay","submitted_at":"2002-12-07T19:00:11Z","abstract_excerpt":"We discuss the solution of accretion disk when the black hole is chosen to be rotating. We study, how the fluid properties get affected for different rotation parameters of the black hole. We know that no cosmic object is static in Universe. Here the effect of the rotation of the black hole to the space-time is considered following an earlier work of the author, where the pseudo-Newtonian potential was prescribed for the Kerr geometry. We show that, with the inclusion of rotation of the black hole, the valid disk parameter region dramatically changes and disk becomes unstable. Also we discuss "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0212186","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/astro-ph/0212186/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":"astro-ph/0212186","created_at":"2026-07-04T16:31:22.620638+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0212186v1","created_at":"2026-07-04T16:31:22.620638+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0212186","created_at":"2026-07-04T16:31:22.620638+00:00"},{"alias_kind":"pith_short_12","alias_value":"LWYLH3C3DZME","created_at":"2026-07-04T16:31:22.620638+00:00"},{"alias_kind":"pith_short_16","alias_value":"LWYLH3C3DZMEKJCG","created_at":"2026-07-04T16:31:22.620638+00:00"},{"alias_kind":"pith_short_8","alias_value":"LWYLH3C3","created_at":"2026-07-04T16:31:22.620638+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"1908.04268","citing_title":"Threshold Drop in Accretion Density if Dark Energy is Accreting onto a Supermassive Black Hole","ref_index":14,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/LWYLH3C3DZMEKJCGCBSDHGSGHH","json":"https://pith.science/pith/LWYLH3C3DZMEKJCGCBSDHGSGHH.json","graph_json":"https://pith.science/api/pith-number/LWYLH3C3DZMEKJCGCBSDHGSGHH/graph.json","events_json":"https://pith.science/api/pith-number/LWYLH3C3DZMEKJCGCBSDHGSGHH/events.json","paper":"https://pith.science/paper/LWYLH3C3"},"agent_actions":{"view_html":"https://pith.science/pith/LWYLH3C3DZMEKJCGCBSDHGSGHH","download_json":"https://pith.science/pith/LWYLH3C3DZMEKJCGCBSDHGSGHH.json","view_paper":"https://pith.science/paper/LWYLH3C3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0212186&json=true","fetch_graph":"https://pith.science/api/pith-number/LWYLH3C3DZMEKJCGCBSDHGSGHH/graph.json","fetch_events":"https://pith.science/api/pith-number/LWYLH3C3DZMEKJCGCBSDHGSGHH/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/LWYLH3C3DZMEKJCGCBSDHGSGHH/action/timestamp_anchor","attest_storage":"https://pith.science/pith/LWYLH3C3DZMEKJCGCBSDHGSGHH/action/storage_attestation","attest_author":"https://pith.science/pith/LWYLH3C3DZMEKJCGCBSDHGSGHH/action/author_attestation","sign_citation":"https://pith.science/pith/LWYLH3C3DZMEKJCGCBSDHGSGHH/action/citation_signature","submit_replication":"https://pith.science/pith/LWYLH3C3DZMEKJCGCBSDHGSGHH/action/replication_record"}},"created_at":"2026-07-04T16:31:22.620638+00:00","updated_at":"2026-07-04T16:31:22.620638+00:00"}