{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:ZKICXAT4GIB7JZ36IN6BTA2ON2","short_pith_number":"pith:ZKICXAT4","schema_version":"1.0","canonical_sha256":"ca902b827c3203f4e77e437c19834e6eb96a018d5891926713ac2c88bac4f435","source":{"kind":"arxiv","id":"1102.1896","version":3},"attestation_state":"computed","paper":{"title":"Amplitudes and lifetimes of solar-like oscillations observed by CoRoT* Red-giant versus main-sequence stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. P. Hatzes, C. Barban, F. Baudin, F. Carrier, J. Ballot, J. De Ridder, K. Belkacem, M.-J. Goupil, O. Benomar, R. Samadi, S. Deheuvels, S. Hekker, T. Kallinger, T. Morel, W. W. Weiss","submitted_at":"2011-02-09T16:22:56Z","abstract_excerpt":"Context. The advent of space-borne missions such as CoRoT or Kepler providing photometric data has brought new possibilities for asteroseismology across the H-R diagram. Solar-like oscillations are now observed in many stars, including red giants and main- sequence stars. Aims. Based on several hundred identified pulsating red giants, we aim to characterize their oscillation amplitudes and widths. These observables are compared with those of main-sequence stars in order to test trends and scaling laws for these parameters for both main-sequence stars and red giants. Methods. An automated fitti"},"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":"1102.1896","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2011-02-09T16:22:56Z","cross_cats_sorted":[],"title_canon_sha256":"ae5ede1b604664e7ef4cea2cfa60b033a7ccae5afbbbcdb5dff6d085ff130a22","abstract_canon_sha256":"884222d29148552a5029d4857e2a132af459cd769b8a199b85de6a0c5d303833"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:03:14.831837Z","signature_b64":"k1EdHPYc/FAyF9C1PxlOjEFNjytk4riyXNRvDoc/pEPPSvDgc5I9Y77sERyZRxEf6y20rICnn+JTBR5O8kcXDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ca902b827c3203f4e77e437c19834e6eb96a018d5891926713ac2c88bac4f435","last_reissued_at":"2026-05-18T02:03:14.831115Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:03:14.831115Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Amplitudes and lifetimes of solar-like oscillations observed by CoRoT* Red-giant versus main-sequence stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. P. Hatzes, C. Barban, F. Baudin, F. Carrier, J. Ballot, J. De Ridder, K. Belkacem, M.-J. Goupil, O. Benomar, R. Samadi, S. Deheuvels, S. Hekker, T. Kallinger, T. Morel, W. W. Weiss","submitted_at":"2011-02-09T16:22:56Z","abstract_excerpt":"Context. The advent of space-borne missions such as CoRoT or Kepler providing photometric data has brought new possibilities for asteroseismology across the H-R diagram. Solar-like oscillations are now observed in many stars, including red giants and main- sequence stars. Aims. Based on several hundred identified pulsating red giants, we aim to characterize their oscillation amplitudes and widths. These observables are compared with those of main-sequence stars in order to test trends and scaling laws for these parameters for both main-sequence stars and red giants. Methods. An automated fitti"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1102.1896","kind":"arxiv","version":3},"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":"1102.1896","created_at":"2026-05-18T02:03:14.831223+00:00"},{"alias_kind":"arxiv_version","alias_value":"1102.1896v3","created_at":"2026-05-18T02:03:14.831223+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1102.1896","created_at":"2026-05-18T02:03:14.831223+00:00"},{"alias_kind":"pith_short_12","alias_value":"ZKICXAT4GIB7","created_at":"2026-05-18T12:26:47.523578+00:00"},{"alias_kind":"pith_short_16","alias_value":"ZKICXAT4GIB7JZ36","created_at":"2026-05-18T12:26:47.523578+00:00"},{"alias_kind":"pith_short_8","alias_value":"ZKICXAT4","created_at":"2026-05-18T12:26:47.523578+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":44,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ZKICXAT4GIB7JZ36IN6BTA2ON2","json":"https://pith.science/pith/ZKICXAT4GIB7JZ36IN6BTA2ON2.json","graph_json":"https://pith.science/api/pith-number/ZKICXAT4GIB7JZ36IN6BTA2ON2/graph.json","events_json":"https://pith.science/api/pith-number/ZKICXAT4GIB7JZ36IN6BTA2ON2/events.json","paper":"https://pith.science/paper/ZKICXAT4"},"agent_actions":{"view_html":"https://pith.science/pith/ZKICXAT4GIB7JZ36IN6BTA2ON2","download_json":"https://pith.science/pith/ZKICXAT4GIB7JZ36IN6BTA2ON2.json","view_paper":"https://pith.science/paper/ZKICXAT4","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1102.1896&json=true","fetch_graph":"https://pith.science/api/pith-number/ZKICXAT4GIB7JZ36IN6BTA2ON2/graph.json","fetch_events":"https://pith.science/api/pith-number/ZKICXAT4GIB7JZ36IN6BTA2ON2/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ZKICXAT4GIB7JZ36IN6BTA2ON2/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ZKICXAT4GIB7JZ36IN6BTA2ON2/action/storage_attestation","attest_author":"https://pith.science/pith/ZKICXAT4GIB7JZ36IN6BTA2ON2/action/author_attestation","sign_citation":"https://pith.science/pith/ZKICXAT4GIB7JZ36IN6BTA2ON2/action/citation_signature","submit_replication":"https://pith.science/pith/ZKICXAT4GIB7JZ36IN6BTA2ON2/action/replication_record"}},"created_at":"2026-05-18T02:03:14.831223+00:00","updated_at":"2026-05-18T02:03:14.831223+00:00"}