{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:DNLN22HILBQDNG3F3EOAHEZZ4F","short_pith_number":"pith:DNLN22HI","schema_version":"1.0","canonical_sha256":"1b56dd68e85860369b65d91c039339e149de46052b451c151f7007808f914e98","source":{"kind":"arxiv","id":"2310.00042","version":3},"attestation_state":"computed","paper":{"title":"Detecting Gravitational Wave Bursts From Stellar-Mass Binaries in the Milli-hertz Band","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA","gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Bence Kocsis, Erez Michaely, Smadar Naoz, Zeyuan Xuan","submitted_at":"2023-09-29T18:00:01Z","abstract_excerpt":"The dynamical formation channels of gravitational wave (GW) sources typically involve a stage when the compact object binary source interacts with the environment, which may excite its eccentricity, yielding efficient GW emission. For the wide eccentric compact object binaries, the GW emission happens mostly near the pericenter passage, creating a unique, burst-like signature in the waveform. This work examines the possibility of stellar-mass bursting sources in the millihertz band for future LISA detections. Because of their long lifetime ($\\sim 10^{7}\\rm\\, yr$) and promising detectability, t"},"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":"2310.00042","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2023-09-29T18:00:01Z","cross_cats_sorted":["astro-ph.GA","gr-qc"],"title_canon_sha256":"7247737e9e2d6e977e6622369fe08f536b61079c7137767dfd7864ff0afbb79c","abstract_canon_sha256":"02327669615ec264d3f10f532f265b667bf699d7943729cedec582b1a9a043c0"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-28T01:04:23.779407Z","signature_b64":"MJVy3lhyB1GIPjDZib4sO5S8XHm+h9zpScdfjZsppDJBMY9igbfKcbupNDfoLuaphvWztxDZON4sJz/Uzj4xDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"1b56dd68e85860369b65d91c039339e149de46052b451c151f7007808f914e98","last_reissued_at":"2026-05-28T01:04:23.778806Z","signature_status":"signed_v1","first_computed_at":"2026-05-28T01:04:23.778806Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Detecting Gravitational Wave Bursts From Stellar-Mass Binaries in the Milli-hertz Band","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA","gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Bence Kocsis, Erez Michaely, Smadar Naoz, Zeyuan Xuan","submitted_at":"2023-09-29T18:00:01Z","abstract_excerpt":"The dynamical formation channels of gravitational wave (GW) sources typically involve a stage when the compact object binary source interacts with the environment, which may excite its eccentricity, yielding efficient GW emission. For the wide eccentric compact object binaries, the GW emission happens mostly near the pericenter passage, creating a unique, burst-like signature in the waveform. This work examines the possibility of stellar-mass bursting sources in the millihertz band for future LISA detections. Because of their long lifetime ($\\sim 10^{7}\\rm\\, yr$) and promising detectability, t"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2310.00042","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/2310.00042/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":"2310.00042","created_at":"2026-05-28T01:04:23.778885+00:00"},{"alias_kind":"arxiv_version","alias_value":"2310.00042v3","created_at":"2026-05-28T01:04:23.778885+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2310.00042","created_at":"2026-05-28T01:04:23.778885+00:00"},{"alias_kind":"pith_short_12","alias_value":"DNLN22HILBQD","created_at":"2026-05-28T01:04:23.778885+00:00"},{"alias_kind":"pith_short_16","alias_value":"DNLN22HILBQDNG3F","created_at":"2026-05-28T01:04:23.778885+00:00"},{"alias_kind":"pith_short_8","alias_value":"DNLN22HI","created_at":"2026-05-28T01:04:23.778885+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.15265","citing_title":"Eccentric Stellar-mass Binary Black Holes: Population, Detectability, and Waveform Analysis in the LISA and LIGO Era","ref_index":50,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/DNLN22HILBQDNG3F3EOAHEZZ4F","json":"https://pith.science/pith/DNLN22HILBQDNG3F3EOAHEZZ4F.json","graph_json":"https://pith.science/api/pith-number/DNLN22HILBQDNG3F3EOAHEZZ4F/graph.json","events_json":"https://pith.science/api/pith-number/DNLN22HILBQDNG3F3EOAHEZZ4F/events.json","paper":"https://pith.science/paper/DNLN22HI"},"agent_actions":{"view_html":"https://pith.science/pith/DNLN22HILBQDNG3F3EOAHEZZ4F","download_json":"https://pith.science/pith/DNLN22HILBQDNG3F3EOAHEZZ4F.json","view_paper":"https://pith.science/paper/DNLN22HI","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2310.00042&json=true","fetch_graph":"https://pith.science/api/pith-number/DNLN22HILBQDNG3F3EOAHEZZ4F/graph.json","fetch_events":"https://pith.science/api/pith-number/DNLN22HILBQDNG3F3EOAHEZZ4F/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/DNLN22HILBQDNG3F3EOAHEZZ4F/action/timestamp_anchor","attest_storage":"https://pith.science/pith/DNLN22HILBQDNG3F3EOAHEZZ4F/action/storage_attestation","attest_author":"https://pith.science/pith/DNLN22HILBQDNG3F3EOAHEZZ4F/action/author_attestation","sign_citation":"https://pith.science/pith/DNLN22HILBQDNG3F3EOAHEZZ4F/action/citation_signature","submit_replication":"https://pith.science/pith/DNLN22HILBQDNG3F3EOAHEZZ4F/action/replication_record"}},"created_at":"2026-05-28T01:04:23.778885+00:00","updated_at":"2026-05-28T01:04:23.778885+00:00"}