{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:YI4QPKYXGL4VSIT7TIJRZH2QWX","short_pith_number":"pith:YI4QPKYX","schema_version":"1.0","canonical_sha256":"c23907ab1732f959227f9a131c9f50b5e1b00e3cf62146d20de0de863477d195","source":{"kind":"arxiv","id":"2410.19087","version":2},"attestation_state":"computed","paper":{"title":"The impact of cosmic ray heating on the cooling of the low-metallicity interstellar medium","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Daniel Seifried, Philipp Girichidis, Pierre Colin N\\\"urnberger, Richard W\\\"unsch, Simon C. O. Glover, Stefanie Walch, Thorsten Naab, Tim-Eric Rathjen, Vittoria Brugaletta","submitted_at":"2024-10-24T18:45:26Z","abstract_excerpt":"Low-metallicity environments are subject to inefficient cooling. They also have low dust-to-gas ratios and therefore less efficient photoelectric (PE) heating than in solar-neighbourhood conditions, where PE heating is one of the most important heating processes in the warm neutral interstellar medium (ISM). We perform magneto-hydrodynamic simulations of stratified ISM patches with a gas metallicity of 0.02 Z$_\\odot$ as part of the SILCC project. The simulations include non-equilibrium chemistry, heating, and cooling of the low-temperature ISM as well as anisotropic cosmic ray (CR) transport, "},"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":"2410.19087","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2024-10-24T18:45:26Z","cross_cats_sorted":[],"title_canon_sha256":"922682e5b2f2a59cade5f5b6a81198413220c6e71bcbfd76eeb1c512aa286bf0","abstract_canon_sha256":"4b6a1632127a967a0c8db8701a612b2621f106e0e8303616d9b483c234f9fc79"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:07:45.720677Z","signature_b64":"i6Bruvvg15iGEC+nJP46e8wCbvsT+kLqhvN0FDVRUhMDw6+6vg9AiSD1eu8gmhDcWTLKQDgG9b7bVewxLPBGDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c23907ab1732f959227f9a131c9f50b5e1b00e3cf62146d20de0de863477d195","last_reissued_at":"2026-07-05T10:07:45.720183Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:07:45.720183Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The impact of cosmic ray heating on the cooling of the low-metallicity interstellar medium","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Daniel Seifried, Philipp Girichidis, Pierre Colin N\\\"urnberger, Richard W\\\"unsch, Simon C. O. Glover, Stefanie Walch, Thorsten Naab, Tim-Eric Rathjen, Vittoria Brugaletta","submitted_at":"2024-10-24T18:45:26Z","abstract_excerpt":"Low-metallicity environments are subject to inefficient cooling. They also have low dust-to-gas ratios and therefore less efficient photoelectric (PE) heating than in solar-neighbourhood conditions, where PE heating is one of the most important heating processes in the warm neutral interstellar medium (ISM). We perform magneto-hydrodynamic simulations of stratified ISM patches with a gas metallicity of 0.02 Z$_\\odot$ as part of the SILCC project. The simulations include non-equilibrium chemistry, heating, and cooling of the low-temperature ISM as well as anisotropic cosmic ray (CR) transport, "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2410.19087","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/2410.19087/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":"2410.19087","created_at":"2026-07-05T10:07:45.720242+00:00"},{"alias_kind":"arxiv_version","alias_value":"2410.19087v2","created_at":"2026-07-05T10:07:45.720242+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2410.19087","created_at":"2026-07-05T10:07:45.720242+00:00"},{"alias_kind":"pith_short_12","alias_value":"YI4QPKYXGL4V","created_at":"2026-07-05T10:07:45.720242+00:00"},{"alias_kind":"pith_short_16","alias_value":"YI4QPKYXGL4VSIT7","created_at":"2026-07-05T10:07:45.720242+00:00"},{"alias_kind":"pith_short_8","alias_value":"YI4QPKYX","created_at":"2026-07-05T10:07:45.720242+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2509.07104","citing_title":"Cosmic Rays on Galaxy Scales: Progress and Pitfalls for CR-MHD Dynamical Models","ref_index":29,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/YI4QPKYXGL4VSIT7TIJRZH2QWX","json":"https://pith.science/pith/YI4QPKYXGL4VSIT7TIJRZH2QWX.json","graph_json":"https://pith.science/api/pith-number/YI4QPKYXGL4VSIT7TIJRZH2QWX/graph.json","events_json":"https://pith.science/api/pith-number/YI4QPKYXGL4VSIT7TIJRZH2QWX/events.json","paper":"https://pith.science/paper/YI4QPKYX"},"agent_actions":{"view_html":"https://pith.science/pith/YI4QPKYXGL4VSIT7TIJRZH2QWX","download_json":"https://pith.science/pith/YI4QPKYXGL4VSIT7TIJRZH2QWX.json","view_paper":"https://pith.science/paper/YI4QPKYX","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2410.19087&json=true","fetch_graph":"https://pith.science/api/pith-number/YI4QPKYXGL4VSIT7TIJRZH2QWX/graph.json","fetch_events":"https://pith.science/api/pith-number/YI4QPKYXGL4VSIT7TIJRZH2QWX/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/YI4QPKYXGL4VSIT7TIJRZH2QWX/action/timestamp_anchor","attest_storage":"https://pith.science/pith/YI4QPKYXGL4VSIT7TIJRZH2QWX/action/storage_attestation","attest_author":"https://pith.science/pith/YI4QPKYXGL4VSIT7TIJRZH2QWX/action/author_attestation","sign_citation":"https://pith.science/pith/YI4QPKYXGL4VSIT7TIJRZH2QWX/action/citation_signature","submit_replication":"https://pith.science/pith/YI4QPKYXGL4VSIT7TIJRZH2QWX/action/replication_record"}},"created_at":"2026-07-05T10:07:45.720242+00:00","updated_at":"2026-07-05T10:07:45.720242+00:00"}