{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:GXF6UEGGDSOOI3LOQLWAYGW2PU","short_pith_number":"pith:GXF6UEGG","schema_version":"1.0","canonical_sha256":"35cbea10c61c9ce46d6e82ec0c1ada7d096d278afc358c5a31993c4ea0699aaf","source":{"kind":"arxiv","id":"1410.3492","version":1},"attestation_state":"computed","paper":{"title":"The Power of Imaging: Constraining the Plasma Properties of GRMHD Simulations using EHT Observations of Sgr A*","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"(2) Institute for Theory, (3) MIT Kavli Institute for Astrophysics, Aleksander Sadowski (3) ((1) Steward Observatory, Chi-kwan Chan (1), Computation, Department of Astronomy, Dimitrios Psaltis (1), Feryal Ozel (1), Harvard-Smithsonian Center for Astrophysics, Ramesh Narayan (2), Space Research), University of Arizona","submitted_at":"2014-10-13T20:03:01Z","abstract_excerpt":"Recent advances in general relativistic magnetohydrodynamic simulations have expanded and improved our understanding of the dynamics of black-hole accretion disks. However, current simulations do not capture the thermodynamics of electrons in the low density accreting plasma. This poses a significant challenge in predicting accretion flow images and spectra from first principles. Because of this, simplified emission models have often been used, with widely different configurations (e.g., disk- versus jet-dominated emission), and were able to account for the observed spectral properties of accr"},"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":"1410.3492","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2014-10-13T20:03:01Z","cross_cats_sorted":[],"title_canon_sha256":"32a65dce8f110ccbdcdb549242e8c55216425b0dfb3fd0434a9e748407e634f0","abstract_canon_sha256":"f8032857491b7dc963b103d5a98b94a3159386ba9c2e8c900205b740da808a47"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:41:48.697096Z","signature_b64":"Hrz3efp0PzcpF/gJA/Dq0j2VfAK08MobSfK44eE9qlbFRErF6f8Ofms1iZwFuvXy4XNiq8PcJiTe6Jfg1UojBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"35cbea10c61c9ce46d6e82ec0c1ada7d096d278afc358c5a31993c4ea0699aaf","last_reissued_at":"2026-05-18T01:41:48.696658Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:41:48.696658Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Power of Imaging: Constraining the Plasma Properties of GRMHD Simulations using EHT Observations of Sgr A*","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"(2) Institute for Theory, (3) MIT Kavli Institute for Astrophysics, Aleksander Sadowski (3) ((1) Steward Observatory, Chi-kwan Chan (1), Computation, Department of Astronomy, Dimitrios Psaltis (1), Feryal Ozel (1), Harvard-Smithsonian Center for Astrophysics, Ramesh Narayan (2), Space Research), University of Arizona","submitted_at":"2014-10-13T20:03:01Z","abstract_excerpt":"Recent advances in general relativistic magnetohydrodynamic simulations have expanded and improved our understanding of the dynamics of black-hole accretion disks. However, current simulations do not capture the thermodynamics of electrons in the low density accreting plasma. This poses a significant challenge in predicting accretion flow images and spectra from first principles. Because of this, simplified emission models have often been used, with widely different configurations (e.g., disk- versus jet-dominated emission), and were able to account for the observed spectral properties of accr"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1410.3492","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":"1410.3492","created_at":"2026-05-18T01:41:48.696719+00:00"},{"alias_kind":"arxiv_version","alias_value":"1410.3492v1","created_at":"2026-05-18T01:41:48.696719+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1410.3492","created_at":"2026-05-18T01:41:48.696719+00:00"},{"alias_kind":"pith_short_12","alias_value":"GXF6UEGGDSOO","created_at":"2026-05-18T12:28:30.664211+00:00"},{"alias_kind":"pith_short_16","alias_value":"GXF6UEGGDSOOI3LO","created_at":"2026-05-18T12:28:30.664211+00:00"},{"alias_kind":"pith_short_8","alias_value":"GXF6UEGG","created_at":"2026-05-18T12:28:30.664211+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2605.16177","citing_title":"Observational signatures of negative mass wormholes through their shadows","ref_index":50,"is_internal_anchor":true},{"citing_arxiv_id":"2605.15166","citing_title":"Polarization Signatures from GRMHD Simulations of Black Hole Accretion","ref_index":64,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/GXF6UEGGDSOOI3LOQLWAYGW2PU","json":"https://pith.science/pith/GXF6UEGGDSOOI3LOQLWAYGW2PU.json","graph_json":"https://pith.science/api/pith-number/GXF6UEGGDSOOI3LOQLWAYGW2PU/graph.json","events_json":"https://pith.science/api/pith-number/GXF6UEGGDSOOI3LOQLWAYGW2PU/events.json","paper":"https://pith.science/paper/GXF6UEGG"},"agent_actions":{"view_html":"https://pith.science/pith/GXF6UEGGDSOOI3LOQLWAYGW2PU","download_json":"https://pith.science/pith/GXF6UEGGDSOOI3LOQLWAYGW2PU.json","view_paper":"https://pith.science/paper/GXF6UEGG","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1410.3492&json=true","fetch_graph":"https://pith.science/api/pith-number/GXF6UEGGDSOOI3LOQLWAYGW2PU/graph.json","fetch_events":"https://pith.science/api/pith-number/GXF6UEGGDSOOI3LOQLWAYGW2PU/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/GXF6UEGGDSOOI3LOQLWAYGW2PU/action/timestamp_anchor","attest_storage":"https://pith.science/pith/GXF6UEGGDSOOI3LOQLWAYGW2PU/action/storage_attestation","attest_author":"https://pith.science/pith/GXF6UEGGDSOOI3LOQLWAYGW2PU/action/author_attestation","sign_citation":"https://pith.science/pith/GXF6UEGGDSOOI3LOQLWAYGW2PU/action/citation_signature","submit_replication":"https://pith.science/pith/GXF6UEGGDSOOI3LOQLWAYGW2PU/action/replication_record"}},"created_at":"2026-05-18T01:41:48.696719+00:00","updated_at":"2026-05-18T01:41:48.696719+00:00"}