{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:CJEB4KKS5DLGPU7WGUJLWN3CJD","short_pith_number":"pith:CJEB4KKS","schema_version":"1.0","canonical_sha256":"12481e2952e8d667d3f63512bb376248f5e1dba224c506e450df22aaa785f564","source":{"kind":"arxiv","id":"2001.05723","version":3},"attestation_state":"computed","paper":{"title":"Gmunu: Toward multigrid based Einstein field equations solver for general-relativistic hydrodynamics simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Lap-Ming Lin, Patrick Chi-Kit Cheong, Tjonnie Guang-Feng Li","submitted_at":"2020-01-16T10:07:47Z","abstract_excerpt":"We present a new open-source axisymmetric general relativistic hydrodynamics code Gmunu (General-relativistic multigrid numerical solver) which uses a multigrid method to solve the elliptic metric equations in the conformally flat condition (CFC) approximation on a spherical grid. Most of the existing relativistic hydrodynamics codes are based on formulations which rely on a free-evolution approach of numerical relativity, where the metric variables are determined by hyperbolic equations without enforcing the constraint equations in the evolution. On the other hand, although a fully constraine"},"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":"2001.05723","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2020-01-16T10:07:47Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"01161162b88d81b6df6061e47ff3fe97b8250cb1573527f72715ddcdd53db4f5","abstract_canon_sha256":"e3bc504879000d8e862d4ccc62c787ff49d2b3051929c4c1369f2727c5155b87"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T01:37:23.324279Z","signature_b64":"RnJyS25d6jzJ+lj45hghYgM3BpzjUhI9I0Uo1rY78H4pZy5t9RNjv6XQma8OMRH5FEbSTZ346vfsTdn5MG7xBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"12481e2952e8d667d3f63512bb376248f5e1dba224c506e450df22aaa785f564","last_reissued_at":"2026-07-05T01:37:23.323875Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T01:37:23.323875Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Gmunu: Toward multigrid based Einstein field equations solver for general-relativistic hydrodynamics simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Lap-Ming Lin, Patrick Chi-Kit Cheong, Tjonnie Guang-Feng Li","submitted_at":"2020-01-16T10:07:47Z","abstract_excerpt":"We present a new open-source axisymmetric general relativistic hydrodynamics code Gmunu (General-relativistic multigrid numerical solver) which uses a multigrid method to solve the elliptic metric equations in the conformally flat condition (CFC) approximation on a spherical grid. Most of the existing relativistic hydrodynamics codes are based on formulations which rely on a free-evolution approach of numerical relativity, where the metric variables are determined by hyperbolic equations without enforcing the constraint equations in the evolution. On the other hand, although a fully constraine"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2001.05723","kind":"arxiv","version":3},"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/2001.05723/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":"2001.05723","created_at":"2026-07-05T01:37:23.323932+00:00"},{"alias_kind":"arxiv_version","alias_value":"2001.05723v3","created_at":"2026-07-05T01:37:23.323932+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2001.05723","created_at":"2026-07-05T01:37:23.323932+00:00"},{"alias_kind":"pith_short_12","alias_value":"CJEB4KKS5DLG","created_at":"2026-07-05T01:37:23.323932+00:00"},{"alias_kind":"pith_short_16","alias_value":"CJEB4KKS5DLGPU7W","created_at":"2026-07-05T01:37:23.323932+00:00"},{"alias_kind":"pith_short_8","alias_value":"CJEB4KKS","created_at":"2026-07-05T01:37:23.323932+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2410.20681","citing_title":"Influence of neutrino-electron scattering and neutrino-pair annihilation on hypermassive neutron star","ref_index":39,"is_internal_anchor":false},{"citing_arxiv_id":"2603.08792","citing_title":"Gamma-ray Signatures of r-Process Radioactivity from the Collapse of Magnetized White Dwarfs","ref_index":44,"is_internal_anchor":false},{"citing_arxiv_id":"2604.23503","citing_title":"Hyperaccreting Neutron Stars inside Massive Envelopes: The Implausibility of Thorne-\\.Zytkow Objects","ref_index":56,"is_internal_anchor":false},{"citing_arxiv_id":"2409.10508","citing_title":"General-relativistic resistive-magnetohydrodynamics simulations of self-consistent magnetized rotating neutron stars","ref_index":53,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/CJEB4KKS5DLGPU7WGUJLWN3CJD","json":"https://pith.science/pith/CJEB4KKS5DLGPU7WGUJLWN3CJD.json","graph_json":"https://pith.science/api/pith-number/CJEB4KKS5DLGPU7WGUJLWN3CJD/graph.json","events_json":"https://pith.science/api/pith-number/CJEB4KKS5DLGPU7WGUJLWN3CJD/events.json","paper":"https://pith.science/paper/CJEB4KKS"},"agent_actions":{"view_html":"https://pith.science/pith/CJEB4KKS5DLGPU7WGUJLWN3CJD","download_json":"https://pith.science/pith/CJEB4KKS5DLGPU7WGUJLWN3CJD.json","view_paper":"https://pith.science/paper/CJEB4KKS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2001.05723&json=true","fetch_graph":"https://pith.science/api/pith-number/CJEB4KKS5DLGPU7WGUJLWN3CJD/graph.json","fetch_events":"https://pith.science/api/pith-number/CJEB4KKS5DLGPU7WGUJLWN3CJD/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/CJEB4KKS5DLGPU7WGUJLWN3CJD/action/timestamp_anchor","attest_storage":"https://pith.science/pith/CJEB4KKS5DLGPU7WGUJLWN3CJD/action/storage_attestation","attest_author":"https://pith.science/pith/CJEB4KKS5DLGPU7WGUJLWN3CJD/action/author_attestation","sign_citation":"https://pith.science/pith/CJEB4KKS5DLGPU7WGUJLWN3CJD/action/citation_signature","submit_replication":"https://pith.science/pith/CJEB4KKS5DLGPU7WGUJLWN3CJD/action/replication_record"}},"created_at":"2026-07-05T01:37:23.323932+00:00","updated_at":"2026-07-05T01:37:23.323932+00:00"}