{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:B2SKJMBH3TOB6H5V34PFNKW6GJ","short_pith_number":"pith:B2SKJMBH","schema_version":"1.0","canonical_sha256":"0ea4a4b027dcdc1f1fb5df1e56aade325f60aa5104d5264303b04bdad28a64b9","source":{"kind":"arxiv","id":"1203.1737","version":2},"attestation_state":"computed","paper":{"title":"Damping rates of solar-like oscillations across the HR diagram. Theoretical calculations confronted to CoRoT and Kepler observations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"F. Baudin, J. P. Marques, K. Belkacem, M. A. Dupret, R. Samadi, T. Appourchaux","submitted_at":"2012-03-08T10:28:48Z","abstract_excerpt":"Space-borne missions CoRoT and {\\it Kepler} are providing a rich harvest of high-quality constraints on solar-like pulsators. Among the seismic parameters, mode damping rates remains poorly understood and thus barely used to infer physical properties of stars. Nevertheless, thanks to CoRoT and {\\it Kepler} space-crafts it is now possible to measure damping rates for hundreds of main-sequence and thousands of red-giant stars with an unprecedented precision.\n  By using a non-adiabatic pulsation code including a time-dependent convection treatment, we compute damping rates for stellar models repr"},"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":"1203.1737","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2012-03-08T10:28:48Z","cross_cats_sorted":[],"title_canon_sha256":"2b3716bfefef144b3a3228a894f34b68e6ea891956056583eb089ed29e0153be","abstract_canon_sha256":"09ea0be36af38c5f9c71970fb62b82fa8e5a0c6f6b8c46b7cce3bec17564e9c0"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:58:50.732550Z","signature_b64":"bB4KLOGWWjs5nhpxxlWD3L/G3MjLLPEu8SZ7Oe91yCJba2ZH4kf8WMEmLBRkCGDau1PIVILir1Mi+JEw07xuAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"0ea4a4b027dcdc1f1fb5df1e56aade325f60aa5104d5264303b04bdad28a64b9","last_reissued_at":"2026-05-18T03:58:50.731897Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:58:50.731897Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Damping rates of solar-like oscillations across the HR diagram. Theoretical calculations confronted to CoRoT and Kepler observations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"F. Baudin, J. P. Marques, K. Belkacem, M. A. Dupret, R. Samadi, T. Appourchaux","submitted_at":"2012-03-08T10:28:48Z","abstract_excerpt":"Space-borne missions CoRoT and {\\it Kepler} are providing a rich harvest of high-quality constraints on solar-like pulsators. Among the seismic parameters, mode damping rates remains poorly understood and thus barely used to infer physical properties of stars. Nevertheless, thanks to CoRoT and {\\it Kepler} space-crafts it is now possible to measure damping rates for hundreds of main-sequence and thousands of red-giant stars with an unprecedented precision.\n  By using a non-adiabatic pulsation code including a time-dependent convection treatment, we compute damping rates for stellar models repr"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1203.1737","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":"1203.1737","created_at":"2026-05-18T03:58:50.731993+00:00"},{"alias_kind":"arxiv_version","alias_value":"1203.1737v2","created_at":"2026-05-18T03:58:50.731993+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1203.1737","created_at":"2026-05-18T03:58:50.731993+00:00"},{"alias_kind":"pith_short_12","alias_value":"B2SKJMBH3TOB","created_at":"2026-05-18T12:26:58.693483+00:00"},{"alias_kind":"pith_short_16","alias_value":"B2SKJMBH3TOB6H5V","created_at":"2026-05-18T12:26:58.693483+00:00"},{"alias_kind":"pith_short_8","alias_value":"B2SKJMBH","created_at":"2026-05-18T12:26:58.693483+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"1906.12262","citing_title":"Asteroseismology of solar-type stars","ref_index":61,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/B2SKJMBH3TOB6H5V34PFNKW6GJ","json":"https://pith.science/pith/B2SKJMBH3TOB6H5V34PFNKW6GJ.json","graph_json":"https://pith.science/api/pith-number/B2SKJMBH3TOB6H5V34PFNKW6GJ/graph.json","events_json":"https://pith.science/api/pith-number/B2SKJMBH3TOB6H5V34PFNKW6GJ/events.json","paper":"https://pith.science/paper/B2SKJMBH"},"agent_actions":{"view_html":"https://pith.science/pith/B2SKJMBH3TOB6H5V34PFNKW6GJ","download_json":"https://pith.science/pith/B2SKJMBH3TOB6H5V34PFNKW6GJ.json","view_paper":"https://pith.science/paper/B2SKJMBH","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1203.1737&json=true","fetch_graph":"https://pith.science/api/pith-number/B2SKJMBH3TOB6H5V34PFNKW6GJ/graph.json","fetch_events":"https://pith.science/api/pith-number/B2SKJMBH3TOB6H5V34PFNKW6GJ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/B2SKJMBH3TOB6H5V34PFNKW6GJ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/B2SKJMBH3TOB6H5V34PFNKW6GJ/action/storage_attestation","attest_author":"https://pith.science/pith/B2SKJMBH3TOB6H5V34PFNKW6GJ/action/author_attestation","sign_citation":"https://pith.science/pith/B2SKJMBH3TOB6H5V34PFNKW6GJ/action/citation_signature","submit_replication":"https://pith.science/pith/B2SKJMBH3TOB6H5V34PFNKW6GJ/action/replication_record"}},"created_at":"2026-05-18T03:58:50.731993+00:00","updated_at":"2026-05-18T03:58:50.731993+00:00"}