{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2007:UY4TSFTEYMNP7GHEKECDXVRWI6","short_pith_number":"pith:UY4TSFTE","schema_version":"1.0","canonical_sha256":"a639391664c31aff98e451043bd63647a58f04ce759bd87de3a0695c0bdb9140","source":{"kind":"arxiv","id":"astro-ph/0703163","version":2},"attestation_state":"computed","paper":{"title":"Origins of Eccentric Extrasolar Planets: Testing the Planet-Planet Scattering Model","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Eric B. Ford (University of Florida), Frederic A. Rasio (Northwestern)","submitted_at":"2007-03-07T23:49:20Z","abstract_excerpt":"(Abridged) In planetary systems with two or more giant planets, dynamical instabilities can lead to collisions or ejections through strong planet--planet scattering. Previous studies for simple initial configurations with two equal-mass planets revealed some discrepancies between the results of numerical simulations and the observed orbital elements of extrasolar planets. Here, we show that simulations with two unequal mass planets starting on nearly circular orbits predict a reduced frequency of collisions and a broader range of final eccentricities. The two-planet scattering model can easily"},"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/0703163","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph","submitted_at":"2007-03-07T23:49:20Z","cross_cats_sorted":[],"title_canon_sha256":"bbaa3c45fb747e5b865eee4b1530089e9f7cd189069b99d037566e3a76ce0066","abstract_canon_sha256":"9a6aadc9f2419e5c0758b8ab8888927d01923cb4724bc238db56fe0e837bc42e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:34:25.341627Z","signature_b64":"6QEr9YJxPUNToZ0jz+VWz/L7BBGO+XWqWkbsh3FOD43/nd25zpDRYao4iyWuMpl2PSvyqbQGaNjvcNMnwCYHDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"a639391664c31aff98e451043bd63647a58f04ce759bd87de3a0695c0bdb9140","last_reissued_at":"2026-07-04T15:34:25.341202Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:34:25.341202Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Origins of Eccentric Extrasolar Planets: Testing the Planet-Planet Scattering Model","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Eric B. Ford (University of Florida), Frederic A. Rasio (Northwestern)","submitted_at":"2007-03-07T23:49:20Z","abstract_excerpt":"(Abridged) In planetary systems with two or more giant planets, dynamical instabilities can lead to collisions or ejections through strong planet--planet scattering. Previous studies for simple initial configurations with two equal-mass planets revealed some discrepancies between the results of numerical simulations and the observed orbital elements of extrasolar planets. Here, we show that simulations with two unequal mass planets starting on nearly circular orbits predict a reduced frequency of collisions and a broader range of final eccentricities. The two-planet scattering model can easily"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0703163","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/astro-ph/0703163/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/0703163","created_at":"2026-07-04T15:34:25.341264+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0703163v2","created_at":"2026-07-04T15:34:25.341264+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0703163","created_at":"2026-07-04T15:34:25.341264+00:00"},{"alias_kind":"pith_short_12","alias_value":"UY4TSFTEYMNP","created_at":"2026-07-04T15:34:25.341264+00:00"},{"alias_kind":"pith_short_16","alias_value":"UY4TSFTEYMNP7GHE","created_at":"2026-07-04T15:34:25.341264+00:00"},{"alias_kind":"pith_short_8","alias_value":"UY4TSFTE","created_at":"2026-07-04T15:34:25.341264+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":8,"internal_anchor_count":8,"sample":[{"citing_arxiv_id":"2607.01027","citing_title":"Understanding eccentric temperate giants: an in-depth study of the architecture and stellar obliquity of the TOI-2134 system","ref_index":95,"is_internal_anchor":true},{"citing_arxiv_id":"2607.01315","citing_title":"Discovery of an Inflated Hot Neptune and Its Formation from Jovian Mass Loss","ref_index":262,"is_internal_anchor":true},{"citing_arxiv_id":"2607.01027","citing_title":"Understanding eccentric temperate giants: an in-depth study of the architecture and stellar obliquity of the TOI-2134 system","ref_index":95,"is_internal_anchor":true},{"citing_arxiv_id":"2606.24114","citing_title":"Kepler Image-Subtracted Light Curves and Variable Star Catalog of NGC 6819","ref_index":186,"is_internal_anchor":true},{"citing_arxiv_id":"2606.23551","citing_title":"Observing a 542-day transiting giant with large TTVs: The 2025 transit of HIP 41378 f and new constraints on the outer system","ref_index":242,"is_internal_anchor":true},{"citing_arxiv_id":"2606.23551","citing_title":"Observing a 542-day transiting giant with large TTVs: The 2025 transit of HIP 41378 f and new constraints on the outer system","ref_index":242,"is_internal_anchor":true},{"citing_arxiv_id":"2606.24114","citing_title":"Kepler Image-Subtracted Light Curves and Variable Star Catalog of NGC 6819","ref_index":186,"is_internal_anchor":true},{"citing_arxiv_id":"2605.14433","citing_title":"Where Do Hot Jupiters Come From? Revisiting Tidal Disruption and Ejection in High-Eccentricity Migration","ref_index":34,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/UY4TSFTEYMNP7GHEKECDXVRWI6","json":"https://pith.science/pith/UY4TSFTEYMNP7GHEKECDXVRWI6.json","graph_json":"https://pith.science/api/pith-number/UY4TSFTEYMNP7GHEKECDXVRWI6/graph.json","events_json":"https://pith.science/api/pith-number/UY4TSFTEYMNP7GHEKECDXVRWI6/events.json","paper":"https://pith.science/paper/UY4TSFTE"},"agent_actions":{"view_html":"https://pith.science/pith/UY4TSFTEYMNP7GHEKECDXVRWI6","download_json":"https://pith.science/pith/UY4TSFTEYMNP7GHEKECDXVRWI6.json","view_paper":"https://pith.science/paper/UY4TSFTE","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0703163&json=true","fetch_graph":"https://pith.science/api/pith-number/UY4TSFTEYMNP7GHEKECDXVRWI6/graph.json","fetch_events":"https://pith.science/api/pith-number/UY4TSFTEYMNP7GHEKECDXVRWI6/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/UY4TSFTEYMNP7GHEKECDXVRWI6/action/timestamp_anchor","attest_storage":"https://pith.science/pith/UY4TSFTEYMNP7GHEKECDXVRWI6/action/storage_attestation","attest_author":"https://pith.science/pith/UY4TSFTEYMNP7GHEKECDXVRWI6/action/author_attestation","sign_citation":"https://pith.science/pith/UY4TSFTEYMNP7GHEKECDXVRWI6/action/citation_signature","submit_replication":"https://pith.science/pith/UY4TSFTEYMNP7GHEKECDXVRWI6/action/replication_record"}},"created_at":"2026-07-04T15:34:25.341264+00:00","updated_at":"2026-07-04T15:34:25.341264+00:00"}