{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:ZEVCSNRRF6Q234YLQXJLKNK2ON","short_pith_number":"pith:ZEVCSNRR","schema_version":"1.0","canonical_sha256":"c92a2936312fa1adf30b85d2b5355a734a0e3a063f1ad5a897570f054d5c9a14","source":{"kind":"arxiv","id":"2305.07652","version":1},"attestation_state":"computed","paper":{"title":"How do supernova remnants cool? -- I. Morphology, optical emission lines, and shocks","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.HE","authors_text":"(2) Institute of Astronomy, (3) Max Planck Institute for Astrophysics, 85748 Garching, Academia Sinica, Astrophysics, D-50937 K\\\"oln, Daniel Seifried (1), Ekaterina I. Makarenko (1), Germany, Germany), Karl-Schwarzschild-Str. 1, No. 1, Pierre C. N\\\"urnberger (1), Roosevelt Rd., Seamus D. Clarke (2), Sec. 4, Stefanie Walch (1), Taipei 10617, Taiwan, Thorsten Naab (3), Tim-Eric Rathjen (1) ((1) I. Physikalisches Institut, Universit\\\"at zu K\\\"oln, Z\\\"ulpicher Str. 77","submitted_at":"2023-05-12T17:59:26Z","abstract_excerpt":"Supernovae (SNe) inject $\\sim 10^{51}$ erg in the interstellar medium, thereby shocking and heating the gas. A substantial fraction of this energy is later lost via radiative cooling. We present a post-processing module for the FLASH code to calculate the cooling radiation from shock-heated gas using collisional excitation data from MAPPINGS V. When applying this tool to a simulated SN remnant (SNR), we find that most energy is emitted in the EUV. However, optical emission lines ($[$O III$]$, $[$N II$]$, $[$S II$]$, H${\\alpha}$, H${\\beta}$) are usually best observable. Our shock detection sche"},"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":"2305.07652","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2023-05-12T17:59:26Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"e8ece4e3d4eb8fc7b4820a1d9b1d5771236ba73e242add6c4dd327f774db1657","abstract_canon_sha256":"234abb4101afe18585dce6fe35c4cb9658f10aee795c0c7bad4a7a069e42a8c8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:12:50.435504Z","signature_b64":"LOtzRP6S/me9J3FjiqBmyXlM7FeMftC3Cy9nmfz6tfHuA2oOFGHnxrxu+pRaTOKhteAFdWn6nYEoSuMVzEnlCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c92a2936312fa1adf30b85d2b5355a734a0e3a063f1ad5a897570f054d5c9a14","last_reissued_at":"2026-07-05T06:12:50.434432Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:12:50.434432Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"How do supernova remnants cool? -- I. Morphology, optical emission lines, and shocks","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.HE","authors_text":"(2) Institute of Astronomy, (3) Max Planck Institute for Astrophysics, 85748 Garching, Academia Sinica, Astrophysics, D-50937 K\\\"oln, Daniel Seifried (1), Ekaterina I. Makarenko (1), Germany, Germany), Karl-Schwarzschild-Str. 1, No. 1, Pierre C. N\\\"urnberger (1), Roosevelt Rd., Seamus D. Clarke (2), Sec. 4, Stefanie Walch (1), Taipei 10617, Taiwan, Thorsten Naab (3), Tim-Eric Rathjen (1) ((1) I. Physikalisches Institut, Universit\\\"at zu K\\\"oln, Z\\\"ulpicher Str. 77","submitted_at":"2023-05-12T17:59:26Z","abstract_excerpt":"Supernovae (SNe) inject $\\sim 10^{51}$ erg in the interstellar medium, thereby shocking and heating the gas. A substantial fraction of this energy is later lost via radiative cooling. We present a post-processing module for the FLASH code to calculate the cooling radiation from shock-heated gas using collisional excitation data from MAPPINGS V. When applying this tool to a simulated SN remnant (SNR), we find that most energy is emitted in the EUV. However, optical emission lines ($[$O III$]$, $[$N II$]$, $[$S II$]$, H${\\alpha}$, H${\\beta}$) are usually best observable. Our shock detection sche"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2305.07652","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/2305.07652/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":"2305.07652","created_at":"2026-07-05T06:12:50.434496+00:00"},{"alias_kind":"arxiv_version","alias_value":"2305.07652v1","created_at":"2026-07-05T06:12:50.434496+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2305.07652","created_at":"2026-07-05T06:12:50.434496+00:00"},{"alias_kind":"pith_short_12","alias_value":"ZEVCSNRRF6Q2","created_at":"2026-07-05T06:12:50.434496+00:00"},{"alias_kind":"pith_short_16","alias_value":"ZEVCSNRRF6Q234YL","created_at":"2026-07-05T06:12:50.434496+00:00"},{"alias_kind":"pith_short_8","alias_value":"ZEVCSNRR","created_at":"2026-07-05T06:12:50.434496+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.04901","citing_title":"FRANZ: Framework for analytical one-zone blastwave dynamics","ref_index":43,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ZEVCSNRRF6Q234YLQXJLKNK2ON","json":"https://pith.science/pith/ZEVCSNRRF6Q234YLQXJLKNK2ON.json","graph_json":"https://pith.science/api/pith-number/ZEVCSNRRF6Q234YLQXJLKNK2ON/graph.json","events_json":"https://pith.science/api/pith-number/ZEVCSNRRF6Q234YLQXJLKNK2ON/events.json","paper":"https://pith.science/paper/ZEVCSNRR"},"agent_actions":{"view_html":"https://pith.science/pith/ZEVCSNRRF6Q234YLQXJLKNK2ON","download_json":"https://pith.science/pith/ZEVCSNRRF6Q234YLQXJLKNK2ON.json","view_paper":"https://pith.science/paper/ZEVCSNRR","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2305.07652&json=true","fetch_graph":"https://pith.science/api/pith-number/ZEVCSNRRF6Q234YLQXJLKNK2ON/graph.json","fetch_events":"https://pith.science/api/pith-number/ZEVCSNRRF6Q234YLQXJLKNK2ON/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ZEVCSNRRF6Q234YLQXJLKNK2ON/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ZEVCSNRRF6Q234YLQXJLKNK2ON/action/storage_attestation","attest_author":"https://pith.science/pith/ZEVCSNRRF6Q234YLQXJLKNK2ON/action/author_attestation","sign_citation":"https://pith.science/pith/ZEVCSNRRF6Q234YLQXJLKNK2ON/action/citation_signature","submit_replication":"https://pith.science/pith/ZEVCSNRRF6Q234YLQXJLKNK2ON/action/replication_record"}},"created_at":"2026-07-05T06:12:50.434496+00:00","updated_at":"2026-07-05T06:12:50.434496+00:00"}