{"paper":{"title":"Where Do Hot Jupiters Come From? Revisiting Tidal Disruption and Ejection in High-Eccentricity Migration","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"Planets with dense cores avoid total tidal disruption in close encounters, allowing more to survive as hot Jupiters or stripped remnants.","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"Qianli Fan, Shang-Fei Liu","submitted_at":"2026-05-14T06:27:25Z","abstract_excerpt":"The origin of hot Jupiters remains a key open question. In the high-eccentricity migration scenario, traditional coreless models predict a strict tidal exclusion zone within $\\sim 2.7$ tidal radii $r_\\textrm{t}$, in which giant planets are either fully disrupted or ejected. We revisit this limit using three-dimensional hydrodynamic simulations of giant planets with realistic dense cores (10 - 20 $M_\\oplus$). We find that even a few-percent-mass core fundamentally changes the outcome: \\textbf{no total disruptions} occur within the previously suggested destruction zone ($\\lesssim 2.7 \\, r_\\textr"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"no total disruptions occur within the previously suggested destruction zone (≲ 2.7 rt). For deep encounters (≲ 1.7 rt) planets suffer severe envelope stripping and are either progressively downsized to dense remnants or ejected after a few close encounters.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The hydrodynamic simulations with 10-20 Earth-mass cores accurately capture the envelope stripping and orbital energy changes without unmodeled effects like magnetic fields or realistic equation of state variations that could alter outcomes.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Planets with realistic dense cores survive close star encounters without total disruption, allowing more to circularize into hot Jupiters or be ejected after mass loss.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Planets with dense cores avoid total tidal disruption in close encounters, allowing more to survive as hot Jupiters or stripped remnants.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"b7f3a544ca30a7620517f2aa2837928731cc9d4ba08c6524b90a085b4eefa6f6"},"source":{"id":"2605.14433","kind":"arxiv","version":1},"verdict":{"id":"59bcc31b-7d18-4300-947e-5d91a4908c59","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-15T02:05:47.922444Z","strongest_claim":"no total disruptions occur within the previously suggested destruction zone (≲ 2.7 rt). For deep encounters (≲ 1.7 rt) planets suffer severe envelope stripping and are either progressively downsized to dense remnants or ejected after a few close encounters.","one_line_summary":"Planets with realistic dense cores survive close star encounters without total disruption, allowing more to circularize into hot Jupiters or be ejected after mass loss.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The hydrodynamic simulations with 10-20 Earth-mass cores accurately capture the envelope stripping and orbital energy changes without unmodeled effects like magnetic fields or realistic equation of state variations that could alter outcomes.","pith_extraction_headline":"Planets with dense cores avoid total tidal disruption in close encounters, allowing more to survive as hot Jupiters or stripped remnants."},"references":{"count":57,"sample":[{"doi":"","year":null,"title":"arXiv e-prints , keywords =","work_id":"cb183557-efa8-41e6-81c2-894809b83586","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1073/pnas.1711406115","year":null,"title":"Proceedings of the National Academy of Sciences , publisher =","work_id":"f84c57d7-7a56-4a5e-8a43-693fa1749021","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.3847/1538-3881/ad60be","year":null,"title":"Surviving in the Hot-Neptune Desert: The Discovery of the Ultrahot Neptune TOI-3261b. , keywords =. doi:10.3847/1538-3881/ad60be , archivePrefix =. 2407.04225 , primaryClass =","work_id":"9ed7637a-eeff-4f8c-bf00-bda93287c8fd","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1038/s41586-019-1470-2","year":2019,"title":"2019, Nature, 572, 355, doi: 10.1038/s41586-019-1470-2","work_id":"af73094e-3157-4db3-a09a-22bf4f042ee6","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":null,"title":"Carter, B. and Luminet, J.-P. , month = may, year =. Tidal compression of a star by a large black hole. Astronomy and Astrophysics , publisher =","work_id":"017d92db-c598-4afe-918c-32b0fee2eab8","ref_index":5,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":57,"snapshot_sha256":"41de15a9c5fc4180c3b9c9babfbb41b0bc5c18f757565f7a8357acc160805ccd","internal_anchors":23},"formal_canon":{"evidence_count":2,"snapshot_sha256":"53bcc0f04ac0ed2e18d460a82eafa8ab955993a9557a1fe26f025352b0d6a0b8"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}