{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:OGLKPHNW6LPLL3I4DAO7MG4YT4","short_pith_number":"pith:OGLKPHNW","schema_version":"1.0","canonical_sha256":"7196a79db6f2deb5ed1c181df61b989f0a2f7c62391625253384b23408990507","source":{"kind":"arxiv","id":"1410.7779","version":1},"attestation_state":"computed","paper":{"title":"Kepler Flares I. Active and Inactive M dwarfs","license":"http://creativecommons.org/licenses/publicdomain/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Adam F. Kowalski, Eric J. Hilton, James R. A. Davenport, John P. Wisniewski, Leslie Hebb, Russell Deitrick, Suzanne L. Hawley","submitted_at":"2014-10-28T20:00:07Z","abstract_excerpt":"We analyzed Kepler short-cadence M dwarf observations. Spectra from the ARC 3.5m telescope identify magnetically active (H$\\alpha$ in emission) stars. The active stars are of mid-M spectral type, have numerous flares, and well-defined rotational modulation due to starspots. The inactive stars are of early-M type, exhibit less starspot signature, and have fewer flares. A Kepler to U-band energy scaling allows comparison of the Kepler flare frequency distributions with previous ground-based data. M dwarfs span a large range of flare frequency and energy, blurring the distinction between active a"},"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":"1410.7779","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/publicdomain/","primary_cat":"astro-ph.SR","submitted_at":"2014-10-28T20:00:07Z","cross_cats_sorted":[],"title_canon_sha256":"49546a39c480ee53b22bd212a8941189c92c45e639432f7355a28420787437a5","abstract_canon_sha256":"c1d6067217e0c356714f6ece0be73bc18e8bd02c902b43c6cff03f636b90f8de"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:41:39.112130Z","signature_b64":"XDOFQFEU2yx5WLLe6nbB8wRHU2rtIpgSZQK6JhI/mGe9OtRwsJ+fs6PERKhoo2wNhAypdtcXM9CcccNce6t0AA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7196a79db6f2deb5ed1c181df61b989f0a2f7c62391625253384b23408990507","last_reissued_at":"2026-05-18T01:41:39.111564Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:41:39.111564Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Kepler Flares I. Active and Inactive M dwarfs","license":"http://creativecommons.org/licenses/publicdomain/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Adam F. Kowalski, Eric J. Hilton, James R. A. Davenport, John P. Wisniewski, Leslie Hebb, Russell Deitrick, Suzanne L. Hawley","submitted_at":"2014-10-28T20:00:07Z","abstract_excerpt":"We analyzed Kepler short-cadence M dwarf observations. Spectra from the ARC 3.5m telescope identify magnetically active (H$\\alpha$ in emission) stars. The active stars are of mid-M spectral type, have numerous flares, and well-defined rotational modulation due to starspots. The inactive stars are of early-M type, exhibit less starspot signature, and have fewer flares. A Kepler to U-band energy scaling allows comparison of the Kepler flare frequency distributions with previous ground-based data. M dwarfs span a large range of flare frequency and energy, blurring the distinction between active a"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1410.7779","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":""},"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":"1410.7779","created_at":"2026-05-18T01:41:39.111636+00:00"},{"alias_kind":"arxiv_version","alias_value":"1410.7779v1","created_at":"2026-05-18T01:41:39.111636+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1410.7779","created_at":"2026-05-18T01:41:39.111636+00:00"},{"alias_kind":"pith_short_12","alias_value":"OGLKPHNW6LPL","created_at":"2026-05-18T12:28:41.024544+00:00"},{"alias_kind":"pith_short_16","alias_value":"OGLKPHNW6LPLL3I4","created_at":"2026-05-18T12:28:41.024544+00:00"},{"alias_kind":"pith_short_8","alias_value":"OGLKPHNW","created_at":"2026-05-18T12:28:41.024544+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":6,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.05468","citing_title":"A single power law for the TRAPPIST-1 flare distribution across four orders of magnitude in energy","ref_index":47,"is_internal_anchor":true},{"citing_arxiv_id":"2605.15587","citing_title":"Rotationally modulated highly circularly polarised radio pulses from the rapidly rotating M dwarf ASKAP J181335-604720","ref_index":20,"is_internal_anchor":false},{"citing_arxiv_id":"2605.02796","citing_title":"Ellipsoidal modulation and multi-wavelength activity in the pre-cataclysmic binary RX J1553.0+4457","ref_index":64,"is_internal_anchor":false},{"citing_arxiv_id":"2605.03939","citing_title":"The Range of Cumulative XUV Flux on GJ 1132 b","ref_index":38,"is_internal_anchor":false},{"citing_arxiv_id":"2605.05468","citing_title":"A single power law for the TRAPPIST-1 flare distribution across four orders of magnitude in energy","ref_index":44,"is_internal_anchor":false},{"citing_arxiv_id":"2605.02796","citing_title":"Ellipsoidal modulation and multi-wavelength activity in the pre-cataclysmic binary RX J1553.0+4457","ref_index":64,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OGLKPHNW6LPLL3I4DAO7MG4YT4","json":"https://pith.science/pith/OGLKPHNW6LPLL3I4DAO7MG4YT4.json","graph_json":"https://pith.science/api/pith-number/OGLKPHNW6LPLL3I4DAO7MG4YT4/graph.json","events_json":"https://pith.science/api/pith-number/OGLKPHNW6LPLL3I4DAO7MG4YT4/events.json","paper":"https://pith.science/paper/OGLKPHNW"},"agent_actions":{"view_html":"https://pith.science/pith/OGLKPHNW6LPLL3I4DAO7MG4YT4","download_json":"https://pith.science/pith/OGLKPHNW6LPLL3I4DAO7MG4YT4.json","view_paper":"https://pith.science/paper/OGLKPHNW","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1410.7779&json=true","fetch_graph":"https://pith.science/api/pith-number/OGLKPHNW6LPLL3I4DAO7MG4YT4/graph.json","fetch_events":"https://pith.science/api/pith-number/OGLKPHNW6LPLL3I4DAO7MG4YT4/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OGLKPHNW6LPLL3I4DAO7MG4YT4/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OGLKPHNW6LPLL3I4DAO7MG4YT4/action/storage_attestation","attest_author":"https://pith.science/pith/OGLKPHNW6LPLL3I4DAO7MG4YT4/action/author_attestation","sign_citation":"https://pith.science/pith/OGLKPHNW6LPLL3I4DAO7MG4YT4/action/citation_signature","submit_replication":"https://pith.science/pith/OGLKPHNW6LPLL3I4DAO7MG4YT4/action/replication_record"}},"created_at":"2026-05-18T01:41:39.111636+00:00","updated_at":"2026-05-18T01:41:39.111636+00:00"}