{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1998:T2DP6SI473BPMI6OF4CS7BBESD","short_pith_number":"pith:T2DP6SI4","schema_version":"1.0","canonical_sha256":"9e86ff491cfec2f623ce2f052f842490f07ee71b1181d8f11c508b7c68c1c320","source":{"kind":"arxiv","id":"astro-ph/9806011","version":1},"attestation_state":"computed","paper":{"title":"Formation of undermassive single white dwarfs and the influence of planets on late stellar evolution","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"G. Nelemans, T.M. Tauris","submitted_at":"1998-05-31T21:55:27Z","abstract_excerpt":"We propose a scenario to form low-mass, single, slow rotating white dwarfs from a solar-like star accompanied by a massive planet, or a brown dwarf, in a relatively close orbit (e.g. HD 89707). Such white dwarfs were recently found by Maxted & Marsh (1998). When the solar-like star ascends the giant branch it captures the planet and the subsequent spiral-in phase expels the envelope of the giant leaving a low-mass helium white dwarf remnant. In case the planet evaporizes, or fills its own Roche-lobe, the outcome is a single undermassive white dwarf. The observed distribution of planetary syste"},"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":"astro-ph/9806011","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1998-05-31T21:55:27Z","cross_cats_sorted":[],"title_canon_sha256":"2f212c86f3896549334e393c210574a02f861ada86f054fb9be814c53a55a5ca","abstract_canon_sha256":"d82bbfdaa9c17eb6c300f4c250945d673ee1c125944fa156cbc6d9faca7838b0"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T14:15:50.967307Z","signature_b64":"Zn2eRHhkGxvD65QLGwkWDdhcK7OuCmA633IFv4m8qGd/mCbuXrkITivbOIFs+HWSyY9+XYrzHOQgPK9GnE2NCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9e86ff491cfec2f623ce2f052f842490f07ee71b1181d8f11c508b7c68c1c320","last_reissued_at":"2026-07-04T14:15:50.966767Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T14:15:50.966767Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Formation of undermassive single white dwarfs and the influence of planets on late stellar evolution","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"G. Nelemans, T.M. Tauris","submitted_at":"1998-05-31T21:55:27Z","abstract_excerpt":"We propose a scenario to form low-mass, single, slow rotating white dwarfs from a solar-like star accompanied by a massive planet, or a brown dwarf, in a relatively close orbit (e.g. HD 89707). Such white dwarfs were recently found by Maxted & Marsh (1998). When the solar-like star ascends the giant branch it captures the planet and the subsequent spiral-in phase expels the envelope of the giant leaving a low-mass helium white dwarf remnant. In case the planet evaporizes, or fills its own Roche-lobe, the outcome is a single undermassive white dwarf. The observed distribution of planetary syste"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9806011","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/astro-ph/9806011/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":"astro-ph/9806011","created_at":"2026-07-04T14:15:50.966852+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9806011v1","created_at":"2026-07-04T14:15:50.966852+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9806011","created_at":"2026-07-04T14:15:50.966852+00:00"},{"alias_kind":"pith_short_12","alias_value":"T2DP6SI473BP","created_at":"2026-07-04T14:15:50.966852+00:00"},{"alias_kind":"pith_short_16","alias_value":"T2DP6SI473BPMI6O","created_at":"2026-07-04T14:15:50.966852+00:00"},{"alias_kind":"pith_short_8","alias_value":"T2DP6SI4","created_at":"2026-07-04T14:15:50.966852+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2608.06204","citing_title":"They Won't Be Giants: Missing Metal-Rich RGB Stars in Gaia Data Indicate Truncated Stellar Evolution","ref_index":45,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/T2DP6SI473BPMI6OF4CS7BBESD","json":"https://pith.science/pith/T2DP6SI473BPMI6OF4CS7BBESD.json","graph_json":"https://pith.science/api/pith-number/T2DP6SI473BPMI6OF4CS7BBESD/graph.json","events_json":"https://pith.science/api/pith-number/T2DP6SI473BPMI6OF4CS7BBESD/events.json","paper":"https://pith.science/paper/T2DP6SI4"},"agent_actions":{"view_html":"https://pith.science/pith/T2DP6SI473BPMI6OF4CS7BBESD","download_json":"https://pith.science/pith/T2DP6SI473BPMI6OF4CS7BBESD.json","view_paper":"https://pith.science/paper/T2DP6SI4","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9806011&json=true","fetch_graph":"https://pith.science/api/pith-number/T2DP6SI473BPMI6OF4CS7BBESD/graph.json","fetch_events":"https://pith.science/api/pith-number/T2DP6SI473BPMI6OF4CS7BBESD/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/T2DP6SI473BPMI6OF4CS7BBESD/action/timestamp_anchor","attest_storage":"https://pith.science/pith/T2DP6SI473BPMI6OF4CS7BBESD/action/storage_attestation","attest_author":"https://pith.science/pith/T2DP6SI473BPMI6OF4CS7BBESD/action/author_attestation","sign_citation":"https://pith.science/pith/T2DP6SI473BPMI6OF4CS7BBESD/action/citation_signature","submit_replication":"https://pith.science/pith/T2DP6SI473BPMI6OF4CS7BBESD/action/replication_record"}},"created_at":"2026-07-04T14:15:50.966852+00:00","updated_at":"2026-07-04T14:15:50.966852+00:00"}