{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:SYBICXRONGUYRNOERCLCT7F2UB","short_pith_number":"pith:SYBICXRO","schema_version":"1.0","canonical_sha256":"9602815e2e69a988b5c4889629fcbaa070a64806a70ee5a725e4acdb4c1b4f4e","source":{"kind":"arxiv","id":"1306.2276","version":2},"attestation_state":"computed","paper":{"title":"Magnetic Coupling in the Disks Around Young Gas Giant Planets","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"M. H. Lee, N. J. Turner, T. Sano","submitted_at":"2013-06-10T18:42:48Z","abstract_excerpt":"We examine the conditions under which the disks of gas and dust orbiting young gas giant planets are sufficiently conducting to experience turbulence driven by the magneto-rotational instability. By modeling the ionization and conductivity in the disk around proto-Jupiter, we find that turbulence is possible if the X-rays emitted near the Sun reach the planet's vicinity and either (1) the gas surface densities are in the range of the minimum-mass models constructed by augmenting Jupiter's satellites to Solar composition, while dust is depleted from the disk atmosphere, or (2) the surface densi"},"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":"1306.2276","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.EP","submitted_at":"2013-06-10T18:42:48Z","cross_cats_sorted":[],"title_canon_sha256":"3d397dbf30f36048da0234bd4e8572717590a65a25a49a013b8fd1880d49ec69","abstract_canon_sha256":"dde9e1ebb4746881de49945a567d229d1c38a26c72802934b809faa41d7edfec"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:59:44.513212Z","signature_b64":"dHzGbKjShzkj5xwYM0cpUfGvxsugjCCXY6cd5K3yzJBm97GHxCBIWqaNT0tuyjjhaijgDPfBxmr5psmL2NEjDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9602815e2e69a988b5c4889629fcbaa070a64806a70ee5a725e4acdb4c1b4f4e","last_reissued_at":"2026-05-18T02:59:44.512467Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:59:44.512467Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Magnetic Coupling in the Disks Around Young Gas Giant Planets","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"M. H. Lee, N. J. Turner, T. Sano","submitted_at":"2013-06-10T18:42:48Z","abstract_excerpt":"We examine the conditions under which the disks of gas and dust orbiting young gas giant planets are sufficiently conducting to experience turbulence driven by the magneto-rotational instability. By modeling the ionization and conductivity in the disk around proto-Jupiter, we find that turbulence is possible if the X-rays emitted near the Sun reach the planet's vicinity and either (1) the gas surface densities are in the range of the minimum-mass models constructed by augmenting Jupiter's satellites to Solar composition, while dust is depleted from the disk atmosphere, or (2) the surface densi"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1306.2276","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":""},"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":"1306.2276","created_at":"2026-05-18T02:59:44.512615+00:00"},{"alias_kind":"arxiv_version","alias_value":"1306.2276v2","created_at":"2026-05-18T02:59:44.512615+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1306.2276","created_at":"2026-05-18T02:59:44.512615+00:00"},{"alias_kind":"pith_short_12","alias_value":"SYBICXRONGUY","created_at":"2026-05-18T12:27:59.945178+00:00"},{"alias_kind":"pith_short_16","alias_value":"SYBICXRONGUYRNOE","created_at":"2026-05-18T12:27:59.945178+00:00"},{"alias_kind":"pith_short_8","alias_value":"SYBICXRO","created_at":"2026-05-18T12:27:59.945178+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.13189","citing_title":"The Accretion Process on Protostars","ref_index":25,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/SYBICXRONGUYRNOERCLCT7F2UB","json":"https://pith.science/pith/SYBICXRONGUYRNOERCLCT7F2UB.json","graph_json":"https://pith.science/api/pith-number/SYBICXRONGUYRNOERCLCT7F2UB/graph.json","events_json":"https://pith.science/api/pith-number/SYBICXRONGUYRNOERCLCT7F2UB/events.json","paper":"https://pith.science/paper/SYBICXRO"},"agent_actions":{"view_html":"https://pith.science/pith/SYBICXRONGUYRNOERCLCT7F2UB","download_json":"https://pith.science/pith/SYBICXRONGUYRNOERCLCT7F2UB.json","view_paper":"https://pith.science/paper/SYBICXRO","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1306.2276&json=true","fetch_graph":"https://pith.science/api/pith-number/SYBICXRONGUYRNOERCLCT7F2UB/graph.json","fetch_events":"https://pith.science/api/pith-number/SYBICXRONGUYRNOERCLCT7F2UB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/SYBICXRONGUYRNOERCLCT7F2UB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/SYBICXRONGUYRNOERCLCT7F2UB/action/storage_attestation","attest_author":"https://pith.science/pith/SYBICXRONGUYRNOERCLCT7F2UB/action/author_attestation","sign_citation":"https://pith.science/pith/SYBICXRONGUYRNOERCLCT7F2UB/action/citation_signature","submit_replication":"https://pith.science/pith/SYBICXRONGUYRNOERCLCT7F2UB/action/replication_record"}},"created_at":"2026-05-18T02:59:44.512615+00:00","updated_at":"2026-05-18T02:59:44.512615+00:00"}