{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:6HDHB3BDY47HZ6MEF36IYKOHS5","short_pith_number":"pith:6HDHB3BD","schema_version":"1.0","canonical_sha256":"f1c670ec23c73e7cf9842efc8c29c7974991b124a37e4ca08e84b1c240a6ec55","source":{"kind":"arxiv","id":"2011.09146","version":2},"attestation_state":"computed","paper":{"title":"Probing the impact of varied migration and gas accretion rates for the formation of giant planets in the pebble accretion scenario","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"Alessandro Morbidelli, Aur\\'elien Crida, Bertram Bitsch, Edward Jurua, Nelson Ndugu","submitted_at":"2020-11-18T07:56:51Z","abstract_excerpt":"The final orbital position of growing planets is determined by their migration speed, which is essentially set by the planetary mass. Small mass planets migrate in type I migration, while more massive planets migrate in type II migration, which is thought to depend mostly on the viscous evolution rate of the disc. A planet is most vulnerable to inward migration before it reaches type II migration and can lose a significant fraction of its semi-major axis at this stage. We investigated the influence of different disc viscosities, the dynamical torque and gas accretion from within the horseshoe "},"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":"2011.09146","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.EP","submitted_at":"2020-11-18T07:56:51Z","cross_cats_sorted":[],"title_canon_sha256":"47f86e86ecef324d8ce8c3d63d5330eee03455b3ade3d4c19a2c454892ff81c7","abstract_canon_sha256":"3e0dcdedfc9b36bff4fbd54cdfab9d173eb3f20cb71743199469e410426e60d4"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T01:58:43.840088Z","signature_b64":"YpC2I75eU/AfvECgKqgsGtiP0KosYeRin9M+CyKkuvlevcvhsKMI9ApPUM7U/uv4zXY6XZhfEQkOsCJdtiL8DQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f1c670ec23c73e7cf9842efc8c29c7974991b124a37e4ca08e84b1c240a6ec55","last_reissued_at":"2026-07-05T01:58:43.839619Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T01:58:43.839619Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Probing the impact of varied migration and gas accretion rates for the formation of giant planets in the pebble accretion scenario","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"Alessandro Morbidelli, Aur\\'elien Crida, Bertram Bitsch, Edward Jurua, Nelson Ndugu","submitted_at":"2020-11-18T07:56:51Z","abstract_excerpt":"The final orbital position of growing planets is determined by their migration speed, which is essentially set by the planetary mass. Small mass planets migrate in type I migration, while more massive planets migrate in type II migration, which is thought to depend mostly on the viscous evolution rate of the disc. A planet is most vulnerable to inward migration before it reaches type II migration and can lose a significant fraction of its semi-major axis at this stage. We investigated the influence of different disc viscosities, the dynamical torque and gas accretion from within the horseshoe "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2011.09146","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/2011.09146/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":"2011.09146","created_at":"2026-07-05T01:58:43.839677+00:00"},{"alias_kind":"arxiv_version","alias_value":"2011.09146v2","created_at":"2026-07-05T01:58:43.839677+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2011.09146","created_at":"2026-07-05T01:58:43.839677+00:00"},{"alias_kind":"pith_short_12","alias_value":"6HDHB3BDY47H","created_at":"2026-07-05T01:58:43.839677+00:00"},{"alias_kind":"pith_short_16","alias_value":"6HDHB3BDY47HZ6ME","created_at":"2026-07-05T01:58:43.839677+00:00"},{"alias_kind":"pith_short_8","alias_value":"6HDHB3BD","created_at":"2026-07-05T01:58:43.839677+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/6HDHB3BDY47HZ6MEF36IYKOHS5","json":"https://pith.science/pith/6HDHB3BDY47HZ6MEF36IYKOHS5.json","graph_json":"https://pith.science/api/pith-number/6HDHB3BDY47HZ6MEF36IYKOHS5/graph.json","events_json":"https://pith.science/api/pith-number/6HDHB3BDY47HZ6MEF36IYKOHS5/events.json","paper":"https://pith.science/paper/6HDHB3BD"},"agent_actions":{"view_html":"https://pith.science/pith/6HDHB3BDY47HZ6MEF36IYKOHS5","download_json":"https://pith.science/pith/6HDHB3BDY47HZ6MEF36IYKOHS5.json","view_paper":"https://pith.science/paper/6HDHB3BD","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2011.09146&json=true","fetch_graph":"https://pith.science/api/pith-number/6HDHB3BDY47HZ6MEF36IYKOHS5/graph.json","fetch_events":"https://pith.science/api/pith-number/6HDHB3BDY47HZ6MEF36IYKOHS5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/6HDHB3BDY47HZ6MEF36IYKOHS5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/6HDHB3BDY47HZ6MEF36IYKOHS5/action/storage_attestation","attest_author":"https://pith.science/pith/6HDHB3BDY47HZ6MEF36IYKOHS5/action/author_attestation","sign_citation":"https://pith.science/pith/6HDHB3BDY47HZ6MEF36IYKOHS5/action/citation_signature","submit_replication":"https://pith.science/pith/6HDHB3BDY47HZ6MEF36IYKOHS5/action/replication_record"}},"created_at":"2026-07-05T01:58:43.839677+00:00","updated_at":"2026-07-05T01:58:43.839677+00:00"}