{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:TZJSWV7J2KZ67APMR26XVK73UG","short_pith_number":"pith:TZJSWV7J","schema_version":"1.0","canonical_sha256":"9e532b57e9d2b3ef81ec8ebd7aabfba18231eec2e929debf02af07aa4ad99bce","source":{"kind":"arxiv","id":"2008.05495","version":1},"attestation_state":"computed","paper":{"title":"Simulations of early kilonova emission from neutron star mergers","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"Daiji Kato, Gediminas Gaigalas, Kyohei Kawaguchi, Masaomi Tanaka, Smaranika Banerjee","submitted_at":"2020-08-12T18:00:36Z","abstract_excerpt":"We present radiative transfer simulations for blue kilonovae hours after neutron star (NS) mergers by performing detailed opacity calculations for the first time. We calculate atomic structures and opacities of highly ionized elements (up to the tenth ionization) with atomic number Z = 20 - 56. We find that the bound-bound transitions of heavy elements are the dominant source of the opacities in the early phase (t < 1 day after the merger), and that the ions with a half-closed electron shell provide the highest contributions. The Planck mean opacity for lanthanide-free ejecta (with electron fr"},"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":"2008.05495","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2020-08-12T18:00:36Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"b0421624b620eef2b4394ca3107bc4af1fa6ab34ca67e003de921e92e47adbfb","abstract_canon_sha256":"e395ad876eddb1687c54f87bac88afb6f1414d067383b625eb69e0fb9721296a"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T01:39:04.928829Z","signature_b64":"TkroM4lqh+tWgmT58ieC2dYTkHurFG5R0U24o14f6PFQSheEyZPM/Uofjs62xUQmwhTHkKM3uZYQBCnOzuxQDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9e532b57e9d2b3ef81ec8ebd7aabfba18231eec2e929debf02af07aa4ad99bce","last_reissued_at":"2026-07-05T01:39:04.928472Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T01:39:04.928472Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Simulations of early kilonova emission from neutron star mergers","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"Daiji Kato, Gediminas Gaigalas, Kyohei Kawaguchi, Masaomi Tanaka, Smaranika Banerjee","submitted_at":"2020-08-12T18:00:36Z","abstract_excerpt":"We present radiative transfer simulations for blue kilonovae hours after neutron star (NS) mergers by performing detailed opacity calculations for the first time. We calculate atomic structures and opacities of highly ionized elements (up to the tenth ionization) with atomic number Z = 20 - 56. We find that the bound-bound transitions of heavy elements are the dominant source of the opacities in the early phase (t < 1 day after the merger), and that the ions with a half-closed electron shell provide the highest contributions. The Planck mean opacity for lanthanide-free ejecta (with electron fr"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2008.05495","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/2008.05495/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":"2008.05495","created_at":"2026-07-05T01:39:04.928531+00:00"},{"alias_kind":"arxiv_version","alias_value":"2008.05495v1","created_at":"2026-07-05T01:39:04.928531+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2008.05495","created_at":"2026-07-05T01:39:04.928531+00:00"},{"alias_kind":"pith_short_12","alias_value":"TZJSWV7J2KZ6","created_at":"2026-07-05T01:39:04.928531+00:00"},{"alias_kind":"pith_short_16","alias_value":"TZJSWV7J2KZ67APM","created_at":"2026-07-05T01:39:04.928531+00:00"},{"alias_kind":"pith_short_8","alias_value":"TZJSWV7J","created_at":"2026-07-05T01:39:04.928531+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.08090","citing_title":"Multi-wavelength Constraints on the Transient EP250905a","ref_index":267,"is_internal_anchor":true},{"citing_arxiv_id":"2606.11299","citing_title":"A magnetar formation in binary neutron star merger","ref_index":11,"is_internal_anchor":false},{"citing_arxiv_id":"2303.15923","citing_title":"Science with the Einstein Telescope: a comparison of different designs","ref_index":68,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/TZJSWV7J2KZ67APMR26XVK73UG","json":"https://pith.science/pith/TZJSWV7J2KZ67APMR26XVK73UG.json","graph_json":"https://pith.science/api/pith-number/TZJSWV7J2KZ67APMR26XVK73UG/graph.json","events_json":"https://pith.science/api/pith-number/TZJSWV7J2KZ67APMR26XVK73UG/events.json","paper":"https://pith.science/paper/TZJSWV7J"},"agent_actions":{"view_html":"https://pith.science/pith/TZJSWV7J2KZ67APMR26XVK73UG","download_json":"https://pith.science/pith/TZJSWV7J2KZ67APMR26XVK73UG.json","view_paper":"https://pith.science/paper/TZJSWV7J","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2008.05495&json=true","fetch_graph":"https://pith.science/api/pith-number/TZJSWV7J2KZ67APMR26XVK73UG/graph.json","fetch_events":"https://pith.science/api/pith-number/TZJSWV7J2KZ67APMR26XVK73UG/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/TZJSWV7J2KZ67APMR26XVK73UG/action/timestamp_anchor","attest_storage":"https://pith.science/pith/TZJSWV7J2KZ67APMR26XVK73UG/action/storage_attestation","attest_author":"https://pith.science/pith/TZJSWV7J2KZ67APMR26XVK73UG/action/author_attestation","sign_citation":"https://pith.science/pith/TZJSWV7J2KZ67APMR26XVK73UG/action/citation_signature","submit_replication":"https://pith.science/pith/TZJSWV7J2KZ67APMR26XVK73UG/action/replication_record"}},"created_at":"2026-07-05T01:39:04.928531+00:00","updated_at":"2026-07-05T01:39:04.928531+00:00"}