{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:BXPBDY6CFUXFY2MZLKFHSHQCXV","short_pith_number":"pith:BXPBDY6C","schema_version":"1.0","canonical_sha256":"0dde11e3c22d2e5c69995a8a791e02bd4bfcccf450fda32ae914b0588f0fb1f4","source":{"kind":"arxiv","id":"2007.14905","version":1},"attestation_state":"computed","paper":{"title":"Retention of Long-Period Gas Giant Planets: Type II Migration Revisited","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"Douglas N. C. Lin, Hui Li, Xiaojia Zhang, Ya-Ping Li, Yi-Xian Chen","submitted_at":"2020-07-29T15:24:03Z","abstract_excerpt":"During their formation, emerging protoplanets tidally interact with their natal disks. Proto-gas-giant planets, with Hills radius larger than the disk thickness, open gaps and quench gas flow in the vicinity of their orbits. It is usually assumed that their type II migration is coupled to the viscous evolution of the disk. Although this hypothesis provides an explanation for the origin of close-in planets, it also encounter predicament on the retention of long-period orbits for most gas giant planets. Moreover, numerical simulations indicate that planets migrations are not solely determined by"},"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":"2007.14905","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.EP","submitted_at":"2020-07-29T15:24:03Z","cross_cats_sorted":[],"title_canon_sha256":"c406766dbbb529fbc2a664a6601725fb4fdc79497cb4b25985e2bd9ed830630c","abstract_canon_sha256":"678b7cc9e7b496c581d6b4cbf03fa71ac3de36b7b8563cab47cc98ef2209b614"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T01:33:41.799045Z","signature_b64":"Pq0QcPy0eQhSeD0h3IA0KKd6POod8wtA3DN50r7j0EV80QZDmf2VUhYYJ0T85+FIR84o1yioJ0MXa61itOwTAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"0dde11e3c22d2e5c69995a8a791e02bd4bfcccf450fda32ae914b0588f0fb1f4","last_reissued_at":"2026-07-05T01:33:41.798684Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T01:33:41.798684Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Retention of Long-Period Gas Giant Planets: Type II Migration Revisited","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"Douglas N. C. Lin, Hui Li, Xiaojia Zhang, Ya-Ping Li, Yi-Xian Chen","submitted_at":"2020-07-29T15:24:03Z","abstract_excerpt":"During their formation, emerging protoplanets tidally interact with their natal disks. Proto-gas-giant planets, with Hills radius larger than the disk thickness, open gaps and quench gas flow in the vicinity of their orbits. It is usually assumed that their type II migration is coupled to the viscous evolution of the disk. Although this hypothesis provides an explanation for the origin of close-in planets, it also encounter predicament on the retention of long-period orbits for most gas giant planets. Moreover, numerical simulations indicate that planets migrations are not solely determined by"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2007.14905","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/2007.14905/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":"2007.14905","created_at":"2026-07-05T01:33:41.798747+00:00"},{"alias_kind":"arxiv_version","alias_value":"2007.14905v1","created_at":"2026-07-05T01:33:41.798747+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2007.14905","created_at":"2026-07-05T01:33:41.798747+00:00"},{"alias_kind":"pith_short_12","alias_value":"BXPBDY6CFUXF","created_at":"2026-07-05T01:33:41.798747+00:00"},{"alias_kind":"pith_short_16","alias_value":"BXPBDY6CFUXFY2MZ","created_at":"2026-07-05T01:33:41.798747+00:00"},{"alias_kind":"pith_short_8","alias_value":"BXPBDY6C","created_at":"2026-07-05T01:33:41.798747+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2501.15874","citing_title":"Effects of Thermodynamics on the Concurrent Accretion and Migration of Gas Giants in Protoplanetary Disks","ref_index":41,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/BXPBDY6CFUXFY2MZLKFHSHQCXV","json":"https://pith.science/pith/BXPBDY6CFUXFY2MZLKFHSHQCXV.json","graph_json":"https://pith.science/api/pith-number/BXPBDY6CFUXFY2MZLKFHSHQCXV/graph.json","events_json":"https://pith.science/api/pith-number/BXPBDY6CFUXFY2MZLKFHSHQCXV/events.json","paper":"https://pith.science/paper/BXPBDY6C"},"agent_actions":{"view_html":"https://pith.science/pith/BXPBDY6CFUXFY2MZLKFHSHQCXV","download_json":"https://pith.science/pith/BXPBDY6CFUXFY2MZLKFHSHQCXV.json","view_paper":"https://pith.science/paper/BXPBDY6C","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2007.14905&json=true","fetch_graph":"https://pith.science/api/pith-number/BXPBDY6CFUXFY2MZLKFHSHQCXV/graph.json","fetch_events":"https://pith.science/api/pith-number/BXPBDY6CFUXFY2MZLKFHSHQCXV/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/BXPBDY6CFUXFY2MZLKFHSHQCXV/action/timestamp_anchor","attest_storage":"https://pith.science/pith/BXPBDY6CFUXFY2MZLKFHSHQCXV/action/storage_attestation","attest_author":"https://pith.science/pith/BXPBDY6CFUXFY2MZLKFHSHQCXV/action/author_attestation","sign_citation":"https://pith.science/pith/BXPBDY6CFUXFY2MZLKFHSHQCXV/action/citation_signature","submit_replication":"https://pith.science/pith/BXPBDY6CFUXFY2MZLKFHSHQCXV/action/replication_record"}},"created_at":"2026-07-05T01:33:41.798747+00:00","updated_at":"2026-07-05T01:33:41.798747+00:00"}