{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:5JRRPBT472QJ262ENJVSKWIIGS","short_pith_number":"pith:5JRRPBT4","schema_version":"1.0","canonical_sha256":"ea6317867cfea09d7b446a6b25590834bdf2a4eb9051be5d0de52798c11967b0","source":{"kind":"arxiv","id":"2204.01412","version":2},"attestation_state":"computed","paper":{"title":"Study of general relativistic magnetohydrodynamic accretion flow around black holes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Debaprasad Maity (IITG), Indu Kalpa Dihingia (IITI), Samik Mitra (IITG), Santabrata Das (IITG)","submitted_at":"2022-04-04T12:02:40Z","abstract_excerpt":"We present a novel approach to study the global structure of steady, axisymmetric, advective, geometrically thin, magnetohydrodynamic (MHD) accretion flow around black holes in full general relativity (GR). Considering ideal MHD conditions and relativistic equation of state (REoS), we solve the governing equations to obtain all possible smooth global accretion solutions. We examine the dynamical and thermodynamical properties of accreting matter in terms of the flow parameters, namely energy (${\\cal E}$), angular momentum (${\\cal L}$), and local magnetic fields. For a thin GRMHD flow, we obser"},"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":"2204.01412","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2022-04-04T12:02:40Z","cross_cats_sorted":[],"title_canon_sha256":"7077117a76f990973b827af56a7c6bdb66600104eaba62a0c6e685c4393a9f19","abstract_canon_sha256":"787caa0e611b6326f80432d76df05d48540178dfb57e51d5d6f261b699657e19"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:03:23.551561Z","signature_b64":"VfkzQ88j0R1DrcuhvPIHxFZMTlbdhy63dsNs4ZipKqCI0wJkvM5RgKTIGHOvRavPzN9UWBzoyfuPUUsgFO8yBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ea6317867cfea09d7b446a6b25590834bdf2a4eb9051be5d0de52798c11967b0","last_reissued_at":"2026-07-05T05:03:23.551101Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:03:23.551101Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Study of general relativistic magnetohydrodynamic accretion flow around black holes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Debaprasad Maity (IITG), Indu Kalpa Dihingia (IITI), Samik Mitra (IITG), Santabrata Das (IITG)","submitted_at":"2022-04-04T12:02:40Z","abstract_excerpt":"We present a novel approach to study the global structure of steady, axisymmetric, advective, geometrically thin, magnetohydrodynamic (MHD) accretion flow around black holes in full general relativity (GR). Considering ideal MHD conditions and relativistic equation of state (REoS), we solve the governing equations to obtain all possible smooth global accretion solutions. We examine the dynamical and thermodynamical properties of accreting matter in terms of the flow parameters, namely energy (${\\cal E}$), angular momentum (${\\cal L}$), and local magnetic fields. For a thin GRMHD flow, we obser"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2204.01412","kind":"arxiv","version":2},"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/2204.01412/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":"2204.01412","created_at":"2026-07-05T05:03:23.551156+00:00"},{"alias_kind":"arxiv_version","alias_value":"2204.01412v2","created_at":"2026-07-05T05:03:23.551156+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2204.01412","created_at":"2026-07-05T05:03:23.551156+00:00"},{"alias_kind":"pith_short_12","alias_value":"5JRRPBT472QJ","created_at":"2026-07-05T05:03:23.551156+00:00"},{"alias_kind":"pith_short_16","alias_value":"5JRRPBT472QJ262E","created_at":"2026-07-05T05:03:23.551156+00:00"},{"alias_kind":"pith_short_8","alias_value":"5JRRPBT4","created_at":"2026-07-05T05:03:23.551156+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2501.07456","citing_title":"Effect of dark matter halo on transonic accretion flow around a galactic black hole","ref_index":71,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/5JRRPBT472QJ262ENJVSKWIIGS","json":"https://pith.science/pith/5JRRPBT472QJ262ENJVSKWIIGS.json","graph_json":"https://pith.science/api/pith-number/5JRRPBT472QJ262ENJVSKWIIGS/graph.json","events_json":"https://pith.science/api/pith-number/5JRRPBT472QJ262ENJVSKWIIGS/events.json","paper":"https://pith.science/paper/5JRRPBT4"},"agent_actions":{"view_html":"https://pith.science/pith/5JRRPBT472QJ262ENJVSKWIIGS","download_json":"https://pith.science/pith/5JRRPBT472QJ262ENJVSKWIIGS.json","view_paper":"https://pith.science/paper/5JRRPBT4","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2204.01412&json=true","fetch_graph":"https://pith.science/api/pith-number/5JRRPBT472QJ262ENJVSKWIIGS/graph.json","fetch_events":"https://pith.science/api/pith-number/5JRRPBT472QJ262ENJVSKWIIGS/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/5JRRPBT472QJ262ENJVSKWIIGS/action/timestamp_anchor","attest_storage":"https://pith.science/pith/5JRRPBT472QJ262ENJVSKWIIGS/action/storage_attestation","attest_author":"https://pith.science/pith/5JRRPBT472QJ262ENJVSKWIIGS/action/author_attestation","sign_citation":"https://pith.science/pith/5JRRPBT472QJ262ENJVSKWIIGS/action/citation_signature","submit_replication":"https://pith.science/pith/5JRRPBT472QJ262ENJVSKWIIGS/action/replication_record"}},"created_at":"2026-07-05T05:03:23.551156+00:00","updated_at":"2026-07-05T05:03:23.551156+00:00"}