{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:HF6OJW6HGTCUCFBALZBZYXDJW5","short_pith_number":"pith:HF6OJW6H","schema_version":"1.0","canonical_sha256":"397ce4dbc734c54114205e439c5c69b777948b162664999fb7108d2ed1ce4236","source":{"kind":"arxiv","id":"2408.01361","version":1},"attestation_state":"computed","paper":{"title":"KHARMA: Flexible, Portable Performance for GRMHD","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Ben S. Prather","submitted_at":"2024-08-02T16:13:49Z","abstract_excerpt":"KHARMA (an acronym for \"Kokkos-based High-Accuracy Relativistic Magnetohydrodynamics with Adaptive mesh refinement\") is a new open-source code for conducting general-relativistic magnetohydrodynamic simulations in stationary spacetimes, primarily of accretion systems. It implements among other options the High-Accuracy Relativistic Magnetohydrodynamics (HARM) scheme, but is written from scratch in C++ with the Kokkos programming model in order to run efficiently on both CPUs and GPUs. In addition to being fast, KHARMA is written to be readable, modular, and extensible, separating functionality"},"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":"2408.01361","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2024-08-02T16:13:49Z","cross_cats_sorted":[],"title_canon_sha256":"0aa529f30f69bbb2d786de91d1eb004d4745cbe4821b99af868fd36a99e48c9b","abstract_canon_sha256":"a1c6b8308537c4c99f55b17300cbb1de58941fdddf15483ea3b24143ae4ae183"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T08:51:30.604028Z","signature_b64":"Wr4Q4D/AnKkN5DguVYg59fFfvyrKX+Hvfx7cG389NJ1SOhCzPzR/r2H08bAdKtXVFUQaCFXr5YSYsUvXs2ydCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"397ce4dbc734c54114205e439c5c69b777948b162664999fb7108d2ed1ce4236","last_reissued_at":"2026-07-05T08:51:30.603573Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T08:51:30.603573Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"KHARMA: Flexible, Portable Performance for GRMHD","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Ben S. Prather","submitted_at":"2024-08-02T16:13:49Z","abstract_excerpt":"KHARMA (an acronym for \"Kokkos-based High-Accuracy Relativistic Magnetohydrodynamics with Adaptive mesh refinement\") is a new open-source code for conducting general-relativistic magnetohydrodynamic simulations in stationary spacetimes, primarily of accretion systems. It implements among other options the High-Accuracy Relativistic Magnetohydrodynamics (HARM) scheme, but is written from scratch in C++ with the Kokkos programming model in order to run efficiently on both CPUs and GPUs. In addition to being fast, KHARMA is written to be readable, modular, and extensible, separating functionality"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2408.01361","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/2408.01361/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":"2408.01361","created_at":"2026-07-05T08:51:30.603629+00:00"},{"alias_kind":"arxiv_version","alias_value":"2408.01361v1","created_at":"2026-07-05T08:51:30.603629+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2408.01361","created_at":"2026-07-05T08:51:30.603629+00:00"},{"alias_kind":"pith_short_12","alias_value":"HF6OJW6HGTCU","created_at":"2026-07-05T08:51:30.603629+00:00"},{"alias_kind":"pith_short_16","alias_value":"HF6OJW6HGTCUCFBA","created_at":"2026-07-05T08:51:30.603629+00:00"},{"alias_kind":"pith_short_8","alias_value":"HF6OJW6H","created_at":"2026-07-05T08:51:30.603629+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":5,"sample":[{"citing_arxiv_id":"2605.28676","citing_title":"Magnetic Configuration Imprints on Quasi-Periodic Variability in GRMHD Simulations of Thin Accretion Disks","ref_index":52,"is_internal_anchor":true},{"citing_arxiv_id":"2606.27591","citing_title":"Exploring the physics behind the observed magnetic filaments in large scale radio galaxies","ref_index":16,"is_internal_anchor":true},{"citing_arxiv_id":"2606.19320","citing_title":"GRMHD and GRRT Simulations of Black Hole Accretion: Flares, Precession, and Complex Spacetimes","ref_index":18,"is_internal_anchor":true},{"citing_arxiv_id":"2603.02520","citing_title":"Observational Properties of Near-Maximally Spinning Supermassive Black Holes","ref_index":33,"is_internal_anchor":true},{"citing_arxiv_id":"2604.15430","citing_title":"GRMHD accretion beyond the black hole paradigm: Light from within the shadow","ref_index":50,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/HF6OJW6HGTCUCFBALZBZYXDJW5","json":"https://pith.science/pith/HF6OJW6HGTCUCFBALZBZYXDJW5.json","graph_json":"https://pith.science/api/pith-number/HF6OJW6HGTCUCFBALZBZYXDJW5/graph.json","events_json":"https://pith.science/api/pith-number/HF6OJW6HGTCUCFBALZBZYXDJW5/events.json","paper":"https://pith.science/paper/HF6OJW6H"},"agent_actions":{"view_html":"https://pith.science/pith/HF6OJW6HGTCUCFBALZBZYXDJW5","download_json":"https://pith.science/pith/HF6OJW6HGTCUCFBALZBZYXDJW5.json","view_paper":"https://pith.science/paper/HF6OJW6H","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2408.01361&json=true","fetch_graph":"https://pith.science/api/pith-number/HF6OJW6HGTCUCFBALZBZYXDJW5/graph.json","fetch_events":"https://pith.science/api/pith-number/HF6OJW6HGTCUCFBALZBZYXDJW5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/HF6OJW6HGTCUCFBALZBZYXDJW5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/HF6OJW6HGTCUCFBALZBZYXDJW5/action/storage_attestation","attest_author":"https://pith.science/pith/HF6OJW6HGTCUCFBALZBZYXDJW5/action/author_attestation","sign_citation":"https://pith.science/pith/HF6OJW6HGTCUCFBALZBZYXDJW5/action/citation_signature","submit_replication":"https://pith.science/pith/HF6OJW6HGTCUCFBALZBZYXDJW5/action/replication_record"}},"created_at":"2026-07-05T08:51:30.603629+00:00","updated_at":"2026-07-05T08:51:30.603629+00:00"}