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How and where these close-in planets formed is one of the major unanswered questions in planet formation. Here we calculate the required disk masses for {\\it in situ} formation of the {\\it Kepler} planets. We find that, if close-in planets formed as {\\it isolation masses}, then standard gas-to-dust ratios yield corresponding gas di"},"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":"1410.1060","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.EP","submitted_at":"2014-10-04T16:45:16Z","cross_cats_sorted":[],"title_canon_sha256":"91cb90db1b4c00ad223422d068cd0331bb0803dce1490c9cc2b34174859a5d5e","abstract_canon_sha256":"46c2ffc092144468c7bebc64d5260dd9398293ca876e55c1a4a938aee4305772"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:41:52.558779Z","signature_b64":"6dujcLnWtgMozWEqM39MLVnSk6TxeFmU7BuAUieycmObAOo5e7dC9p1Jx95OC4RBOAyR9cqaX0KbW9UEq7QZAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"914beda8c964c4662f102f9277858b51dcbfcf4449131aac0f27ca11da094f55","last_reissued_at":"2026-05-18T01:41:52.558084Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:41:52.558084Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Formation of close in Super-Earths \\& Mini-Neptunes: Required Disk Masses \\& Their Implications","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"Hilke E. 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