{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:MDNG5FHPDYQEAQ4GKL3U2SDPPJ","short_pith_number":"pith:MDNG5FHP","schema_version":"1.0","canonical_sha256":"60da6e94ef1e2040438652f74d486f7a6281f89e55001be17a1913f3c8a18c49","source":{"kind":"arxiv","id":"2410.08330","version":1},"attestation_state":"computed","paper":{"title":"Connecting integrated RGB mass loss from asteroseismology and globular clusters","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. Miglio, E. Willett, J. S. Thomsen, K. Brogaard, W. E. van Rossem","submitted_at":"2024-10-10T19:40:14Z","abstract_excerpt":"Context. Asteroseismic investigations of solar-like oscillations in giant stars enable the derivation of their masses and radii. For mono-age mono-metallicity populations of stars this allows the integrated red giant branch (RGB) mass loss to be estimated by comparing the median mass of the low-luminosity RGB stars to that of the helium-core-burning stars (HeCB). Aims. We aim to exploit quasi mono-age mono-metallicity populations of field stars in the $\\alpha$-rich sequence of the Milky Way (MW) to derive the integrated mass loss and its dependence on metallicity. By comparing to metal-rich gl"},"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":"2410.08330","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.SR","submitted_at":"2024-10-10T19:40:14Z","cross_cats_sorted":[],"title_canon_sha256":"f86f74849ac5242b691ada48a7b55cc353b496a5df4fb8854b8043501ca897d0","abstract_canon_sha256":"95d933757874b2bfa2e1e51eb83becab168aaf18d6aaf556c6be41e6c1d2a36f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T09:37:41.975253Z","signature_b64":"DvrMHBec96lhHS3QiembQ3U96lrQyHLCijFWcPUqchS3LQZQpQRS9X1cPRtBqTnpADwF02aPuunybphljMWBCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"60da6e94ef1e2040438652f74d486f7a6281f89e55001be17a1913f3c8a18c49","last_reissued_at":"2026-07-05T09:37:41.974722Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T09:37:41.974722Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Connecting integrated RGB mass loss from asteroseismology and globular clusters","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. Miglio, E. Willett, J. S. Thomsen, K. Brogaard, W. E. van Rossem","submitted_at":"2024-10-10T19:40:14Z","abstract_excerpt":"Context. Asteroseismic investigations of solar-like oscillations in giant stars enable the derivation of their masses and radii. For mono-age mono-metallicity populations of stars this allows the integrated red giant branch (RGB) mass loss to be estimated by comparing the median mass of the low-luminosity RGB stars to that of the helium-core-burning stars (HeCB). Aims. We aim to exploit quasi mono-age mono-metallicity populations of field stars in the $\\alpha$-rich sequence of the Milky Way (MW) to derive the integrated mass loss and its dependence on metallicity. By comparing to metal-rich gl"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2410.08330","kind":"arxiv","version":1},"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/2410.08330/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":"2410.08330","created_at":"2026-07-05T09:37:41.974785+00:00"},{"alias_kind":"arxiv_version","alias_value":"2410.08330v1","created_at":"2026-07-05T09:37:41.974785+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2410.08330","created_at":"2026-07-05T09:37:41.974785+00:00"},{"alias_kind":"pith_short_12","alias_value":"MDNG5FHPDYQE","created_at":"2026-07-05T09:37:41.974785+00:00"},{"alias_kind":"pith_short_16","alias_value":"MDNG5FHPDYQEAQ4G","created_at":"2026-07-05T09:37:41.974785+00:00"},{"alias_kind":"pith_short_8","alias_value":"MDNG5FHP","created_at":"2026-07-05T09:37:41.974785+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2608.10909","citing_title":"Pulsation periods reveal tension between theoretical and empirical radii for classical Cepheids in eclipsing binary systems","ref_index":68,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MDNG5FHPDYQEAQ4GKL3U2SDPPJ","json":"https://pith.science/pith/MDNG5FHPDYQEAQ4GKL3U2SDPPJ.json","graph_json":"https://pith.science/api/pith-number/MDNG5FHPDYQEAQ4GKL3U2SDPPJ/graph.json","events_json":"https://pith.science/api/pith-number/MDNG5FHPDYQEAQ4GKL3U2SDPPJ/events.json","paper":"https://pith.science/paper/MDNG5FHP"},"agent_actions":{"view_html":"https://pith.science/pith/MDNG5FHPDYQEAQ4GKL3U2SDPPJ","download_json":"https://pith.science/pith/MDNG5FHPDYQEAQ4GKL3U2SDPPJ.json","view_paper":"https://pith.science/paper/MDNG5FHP","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2410.08330&json=true","fetch_graph":"https://pith.science/api/pith-number/MDNG5FHPDYQEAQ4GKL3U2SDPPJ/graph.json","fetch_events":"https://pith.science/api/pith-number/MDNG5FHPDYQEAQ4GKL3U2SDPPJ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MDNG5FHPDYQEAQ4GKL3U2SDPPJ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MDNG5FHPDYQEAQ4GKL3U2SDPPJ/action/storage_attestation","attest_author":"https://pith.science/pith/MDNG5FHPDYQEAQ4GKL3U2SDPPJ/action/author_attestation","sign_citation":"https://pith.science/pith/MDNG5FHPDYQEAQ4GKL3U2SDPPJ/action/citation_signature","submit_replication":"https://pith.science/pith/MDNG5FHPDYQEAQ4GKL3U2SDPPJ/action/replication_record"}},"created_at":"2026-07-05T09:37:41.974785+00:00","updated_at":"2026-07-05T09:37:41.974785+00:00"}