{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2007:MHVXAW6DXNKNQI3SAYEIZT6VQ2","short_pith_number":"pith:MHVXAW6D","schema_version":"1.0","canonical_sha256":"61eb705bc3bb54d8237206088ccfd5869452820942deff7c48a0da109d3d44af","source":{"kind":"arxiv","id":"0707.2733","version":1},"attestation_state":"computed","paper":{"title":"Origin of the Metallicity Dependence of Exoplanet Host Stars in the Protoplanetary Disk Mass Distribution","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"C. J. Clarke, J. S. Greaves, M. C. Wyatt","submitted_at":"2007-07-18T14:51:16Z","abstract_excerpt":"The probability of a star hosting a planet that is detectable in radial velocity surveys increases Ppl(Z) oc 10^2Z, where Z is metallicity. Core accretion models reproduce this trend, since the protoplanetary disk of a high metallicity star has a high density of solids and so forms cores which accrete gas before the primordial gas disk dissipates. This paper considers the origin of the form of Ppl(Z). We introduce a simple model in which detectable planets form when the mass of solids in the protoplanetary disk, Ms, exceeds a critical value. In this model the form of Ppl(Z) is a direct reflect"},"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":"0707.2733","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2007-07-18T14:51:16Z","cross_cats_sorted":[],"title_canon_sha256":"b2524dd4626c7952160727e69f93e77d827bd48b07237e1c71825d1f61147089","abstract_canon_sha256":"ad204a04b5ee520ea2796de320194d7182fa49bfaeed0496cbeff0e1d46e45ce"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:03:08.597515Z","signature_b64":"522//Ij1/rhetIlWpucuSfkjrgrvkqdWxVdrDxSyXh+kioEraXJw9TupsOrx1SYU0BargRcg/fi6xF/KVPsJBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"61eb705bc3bb54d8237206088ccfd5869452820942deff7c48a0da109d3d44af","last_reissued_at":"2026-07-04T15:03:08.597146Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:03:08.597146Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Origin of the Metallicity Dependence of Exoplanet Host Stars in the Protoplanetary Disk Mass Distribution","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"C. J. Clarke, J. S. Greaves, M. C. Wyatt","submitted_at":"2007-07-18T14:51:16Z","abstract_excerpt":"The probability of a star hosting a planet that is detectable in radial velocity surveys increases Ppl(Z) oc 10^2Z, where Z is metallicity. Core accretion models reproduce this trend, since the protoplanetary disk of a high metallicity star has a high density of solids and so forms cores which accrete gas before the primordial gas disk dissipates. This paper considers the origin of the form of Ppl(Z). We introduce a simple model in which detectable planets form when the mass of solids in the protoplanetary disk, Ms, exceeds a critical value. In this model the form of Ppl(Z) is a direct reflect"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0707.2733","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/0707.2733/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":"0707.2733","created_at":"2026-07-04T15:03:08.597213+00:00"},{"alias_kind":"arxiv_version","alias_value":"0707.2733v1","created_at":"2026-07-04T15:03:08.597213+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0707.2733","created_at":"2026-07-04T15:03:08.597213+00:00"},{"alias_kind":"pith_short_12","alias_value":"MHVXAW6DXNKN","created_at":"2026-07-04T15:03:08.597213+00:00"},{"alias_kind":"pith_short_16","alias_value":"MHVXAW6DXNKNQI3S","created_at":"2026-07-04T15:03:08.597213+00:00"},{"alias_kind":"pith_short_8","alias_value":"MHVXAW6D","created_at":"2026-07-04T15:03:08.597213+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2412.16278","citing_title":"Correlation between planet formation rate and gas surface density: an analog of Kennicutt Schmidt law for planet formation","ref_index":41,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MHVXAW6DXNKNQI3SAYEIZT6VQ2","json":"https://pith.science/pith/MHVXAW6DXNKNQI3SAYEIZT6VQ2.json","graph_json":"https://pith.science/api/pith-number/MHVXAW6DXNKNQI3SAYEIZT6VQ2/graph.json","events_json":"https://pith.science/api/pith-number/MHVXAW6DXNKNQI3SAYEIZT6VQ2/events.json","paper":"https://pith.science/paper/MHVXAW6D"},"agent_actions":{"view_html":"https://pith.science/pith/MHVXAW6DXNKNQI3SAYEIZT6VQ2","download_json":"https://pith.science/pith/MHVXAW6DXNKNQI3SAYEIZT6VQ2.json","view_paper":"https://pith.science/paper/MHVXAW6D","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0707.2733&json=true","fetch_graph":"https://pith.science/api/pith-number/MHVXAW6DXNKNQI3SAYEIZT6VQ2/graph.json","fetch_events":"https://pith.science/api/pith-number/MHVXAW6DXNKNQI3SAYEIZT6VQ2/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MHVXAW6DXNKNQI3SAYEIZT6VQ2/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MHVXAW6DXNKNQI3SAYEIZT6VQ2/action/storage_attestation","attest_author":"https://pith.science/pith/MHVXAW6DXNKNQI3SAYEIZT6VQ2/action/author_attestation","sign_citation":"https://pith.science/pith/MHVXAW6DXNKNQI3SAYEIZT6VQ2/action/citation_signature","submit_replication":"https://pith.science/pith/MHVXAW6DXNKNQI3SAYEIZT6VQ2/action/replication_record"}},"created_at":"2026-07-04T15:03:08.597213+00:00","updated_at":"2026-07-04T15:03:08.597213+00:00"}