{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:K3RQMNEEZRB5V7GSP63DOO4X2K","short_pith_number":"pith:K3RQMNEE","schema_version":"1.0","canonical_sha256":"56e3063484cc43dafcd27fb6373b97d2ba833b020067ae5bee074d1e9418a62e","source":{"kind":"arxiv","id":"2209.01909","version":2},"attestation_state":"computed","paper":{"title":"The contribution of binary star formation via core-fragmentation on protostellar multiplicity","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"R. Kuruwita, T. Haugb{\\o}lle","submitted_at":"2022-09-05T11:16:10Z","abstract_excerpt":"Observations of young multiple star systems find a bimodal distribution in companion frequency and separation. The origin of these peaks has often been attributed to binary formation via core and disc fragmentation. However, theory and simulations suggest that young stellar systems that form via core fragmentation undergo significant orbital evolution. We investigate the influence of the environment on the formation and orbital evolution of multiple star systems, and how core fragmentation contributes to the formation of close (20-100AU) binaries. We use multiple simulations of star formation "},"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":"2209.01909","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2022-09-05T11:16:10Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"9abd864c9e066ff8d6e35d090a7c5ae79632c13c87029a48eaab8f8e67a12772","abstract_canon_sha256":"271dcb1c7c84186a4e3a8c62774a10ac38621cbc6fca4b51267fa8e6b89c59f1"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:22:41.707898Z","signature_b64":"rARJwE6gCRd2MJOnCJCPGjH4ULne6tGL6xxiXJB0V4tA7qTMsfWYNuglW4Ykyd194eHg6ayk+QoJ9d5sreDSDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"56e3063484cc43dafcd27fb6373b97d2ba833b020067ae5bee074d1e9418a62e","last_reissued_at":"2026-07-05T06:22:41.707402Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:22:41.707402Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The contribution of binary star formation via core-fragmentation on protostellar multiplicity","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"R. Kuruwita, T. Haugb{\\o}lle","submitted_at":"2022-09-05T11:16:10Z","abstract_excerpt":"Observations of young multiple star systems find a bimodal distribution in companion frequency and separation. The origin of these peaks has often been attributed to binary formation via core and disc fragmentation. However, theory and simulations suggest that young stellar systems that form via core fragmentation undergo significant orbital evolution. We investigate the influence of the environment on the formation and orbital evolution of multiple star systems, and how core fragmentation contributes to the formation of close (20-100AU) binaries. We use multiple simulations of star formation "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2209.01909","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/2209.01909/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":"2209.01909","created_at":"2026-07-05T06:22:41.707463+00:00"},{"alias_kind":"arxiv_version","alias_value":"2209.01909v2","created_at":"2026-07-05T06:22:41.707463+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2209.01909","created_at":"2026-07-05T06:22:41.707463+00:00"},{"alias_kind":"pith_short_12","alias_value":"K3RQMNEEZRB5","created_at":"2026-07-05T06:22:41.707463+00:00"},{"alias_kind":"pith_short_16","alias_value":"K3RQMNEEZRB5V7GS","created_at":"2026-07-05T06:22:41.707463+00:00"},{"alias_kind":"pith_short_8","alias_value":"K3RQMNEE","created_at":"2026-07-05T06:22:41.707463+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.28159","citing_title":"Southern Massive Stars at High Angular Resolution (SMaSH+): Properties of hierarchical massive triples","ref_index":86,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/K3RQMNEEZRB5V7GSP63DOO4X2K","json":"https://pith.science/pith/K3RQMNEEZRB5V7GSP63DOO4X2K.json","graph_json":"https://pith.science/api/pith-number/K3RQMNEEZRB5V7GSP63DOO4X2K/graph.json","events_json":"https://pith.science/api/pith-number/K3RQMNEEZRB5V7GSP63DOO4X2K/events.json","paper":"https://pith.science/paper/K3RQMNEE"},"agent_actions":{"view_html":"https://pith.science/pith/K3RQMNEEZRB5V7GSP63DOO4X2K","download_json":"https://pith.science/pith/K3RQMNEEZRB5V7GSP63DOO4X2K.json","view_paper":"https://pith.science/paper/K3RQMNEE","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2209.01909&json=true","fetch_graph":"https://pith.science/api/pith-number/K3RQMNEEZRB5V7GSP63DOO4X2K/graph.json","fetch_events":"https://pith.science/api/pith-number/K3RQMNEEZRB5V7GSP63DOO4X2K/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/K3RQMNEEZRB5V7GSP63DOO4X2K/action/timestamp_anchor","attest_storage":"https://pith.science/pith/K3RQMNEEZRB5V7GSP63DOO4X2K/action/storage_attestation","attest_author":"https://pith.science/pith/K3RQMNEEZRB5V7GSP63DOO4X2K/action/author_attestation","sign_citation":"https://pith.science/pith/K3RQMNEEZRB5V7GSP63DOO4X2K/action/citation_signature","submit_replication":"https://pith.science/pith/K3RQMNEEZRB5V7GSP63DOO4X2K/action/replication_record"}},"created_at":"2026-07-05T06:22:41.707463+00:00","updated_at":"2026-07-05T06:22:41.707463+00:00"}