{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:YFUTISSZ4LQGNLFT5Q62BJ477P","short_pith_number":"pith:YFUTISSZ","schema_version":"1.0","canonical_sha256":"c169344a59e2e066acb3ec3da0a79ffbdccf5cd9224de627e704442cbc6f0256","source":{"kind":"arxiv","id":"2401.04172","version":2},"attestation_state":"computed","paper":{"title":"Equations of State, Thermodynamics, and Miscibility Curves for Jovian Planet and Giant Exoplanet Evolutionary Models","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.EP","authors_text":"Adam Burrows, Ankan Sur, Roberto Tejada Arevalo, Yubo Su","submitted_at":"2024-01-08T19:00:04Z","abstract_excerpt":"The equation of state of hydrogen-helium (H-He) mixtures plays a vital role in the evolution and structure of gas giant planets and exoplanets. Recent equations of state that account for hydrogen-helium interactions, coupled with hydrogen-helium immiscibility curves, can now produce more physical evolutionary models, such as accounting for helium rain with greater fidelity than in the past. In this work, we present a set of tools for planetary evolution\\footnote{All tables of thermodynamic quantities and derivatives are available at \\url{https://github.com/Rob685/hhe_eos_misc}, along with a un"},"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":"2401.04172","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.EP","submitted_at":"2024-01-08T19:00:04Z","cross_cats_sorted":["astro-ph.IM"],"title_canon_sha256":"69fc9f2ff919465e4a59d27aa23ca95c69013a7ab168bd8cd42668b4ac84ad42","abstract_canon_sha256":"8e756abe3f7b240c2bd30c0a4ee750e5f4f8c1659138339528c4c5a20c31ebd1"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T08:53:19.173849Z","signature_b64":"Uq7HauCtvhNoV/3Do8e6zMwpNLulZjiaJhm2MgRhHxpbNe+62FtI1XxrPhDu+Pk52RqCqzZ2MIrvCeZHvttDBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c169344a59e2e066acb3ec3da0a79ffbdccf5cd9224de627e704442cbc6f0256","last_reissued_at":"2026-07-05T08:53:19.173375Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T08:53:19.173375Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Equations of State, Thermodynamics, and Miscibility Curves for Jovian Planet and Giant Exoplanet Evolutionary Models","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.EP","authors_text":"Adam Burrows, Ankan Sur, Roberto Tejada Arevalo, Yubo Su","submitted_at":"2024-01-08T19:00:04Z","abstract_excerpt":"The equation of state of hydrogen-helium (H-He) mixtures plays a vital role in the evolution and structure of gas giant planets and exoplanets. Recent equations of state that account for hydrogen-helium interactions, coupled with hydrogen-helium immiscibility curves, can now produce more physical evolutionary models, such as accounting for helium rain with greater fidelity than in the past. In this work, we present a set of tools for planetary evolution\\footnote{All tables of thermodynamic quantities and derivatives are available at \\url{https://github.com/Rob685/hhe_eos_misc}, along with a un"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2401.04172","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/2401.04172/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":"2401.04172","created_at":"2026-07-05T08:53:19.173425+00:00"},{"alias_kind":"arxiv_version","alias_value":"2401.04172v2","created_at":"2026-07-05T08:53:19.173425+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2401.04172","created_at":"2026-07-05T08:53:19.173425+00:00"},{"alias_kind":"pith_short_12","alias_value":"YFUTISSZ4LQG","created_at":"2026-07-05T08:53:19.173425+00:00"},{"alias_kind":"pith_short_16","alias_value":"YFUTISSZ4LQGNLFT","created_at":"2026-07-05T08:53:19.173425+00:00"},{"alias_kind":"pith_short_8","alias_value":"YFUTISSZ","created_at":"2026-07-05T08:53:19.173425+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.23602","citing_title":"Data analysis methods for powder x-ray diffraction intensity under laser-driven dynamic compression at Omega and NIF laser facilities","ref_index":218,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/YFUTISSZ4LQGNLFT5Q62BJ477P","json":"https://pith.science/pith/YFUTISSZ4LQGNLFT5Q62BJ477P.json","graph_json":"https://pith.science/api/pith-number/YFUTISSZ4LQGNLFT5Q62BJ477P/graph.json","events_json":"https://pith.science/api/pith-number/YFUTISSZ4LQGNLFT5Q62BJ477P/events.json","paper":"https://pith.science/paper/YFUTISSZ"},"agent_actions":{"view_html":"https://pith.science/pith/YFUTISSZ4LQGNLFT5Q62BJ477P","download_json":"https://pith.science/pith/YFUTISSZ4LQGNLFT5Q62BJ477P.json","view_paper":"https://pith.science/paper/YFUTISSZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2401.04172&json=true","fetch_graph":"https://pith.science/api/pith-number/YFUTISSZ4LQGNLFT5Q62BJ477P/graph.json","fetch_events":"https://pith.science/api/pith-number/YFUTISSZ4LQGNLFT5Q62BJ477P/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/YFUTISSZ4LQGNLFT5Q62BJ477P/action/timestamp_anchor","attest_storage":"https://pith.science/pith/YFUTISSZ4LQGNLFT5Q62BJ477P/action/storage_attestation","attest_author":"https://pith.science/pith/YFUTISSZ4LQGNLFT5Q62BJ477P/action/author_attestation","sign_citation":"https://pith.science/pith/YFUTISSZ4LQGNLFT5Q62BJ477P/action/citation_signature","submit_replication":"https://pith.science/pith/YFUTISSZ4LQGNLFT5Q62BJ477P/action/replication_record"}},"created_at":"2026-07-05T08:53:19.173425+00:00","updated_at":"2026-07-05T08:53:19.173425+00:00"}