{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:3QX6RWXEB4YFG6P3HQYFGX2TEX","short_pith_number":"pith:3QX6RWXE","schema_version":"1.0","canonical_sha256":"dc2fe8dae40f305379fb3c30535f5325c961a9c1d9af32162c4ae534ce9f8b43","source":{"kind":"arxiv","id":"1704.06689","version":1},"attestation_state":"computed","paper":{"title":"Mass Loss Rates from Coronal Mass Ejections: A Predictive Theoretical Model for Solar-Type Stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Steven R. Cranmer (CU Boulder)","submitted_at":"2017-04-21T19:31:30Z","abstract_excerpt":"Coronal mass ejections (CMEs) are eruptive events that cause a solar-type star to shed mass and magnetic flux. CMEs tend to occur together with flares, radio storms, and bursts of energetic particles. On the Sun, CME-related mass loss is roughly an order of magnitude less intense than that of the background solar wind. However, on other types of stars, CMEs have been proposed to carry away much more mass and energy than the time-steady wind. Earlier papers have used observed correlations between solar CMEs and flare energies, in combination with stellar flare observations, to estimate stellar "},"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":"1704.06689","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2017-04-21T19:31:30Z","cross_cats_sorted":[],"title_canon_sha256":"6924605704e3a68384bfdde2bdf42241db06b0051ec22cb9667db14f51b16553","abstract_canon_sha256":"0bab6762ea7684bbc8f7646f2264e256b415232fc4ca46dbc3a7895763a707b5"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:43:50.309108Z","signature_b64":"qanGrT5JZJaqxGl9HnLOP5vGRFBD4k82UksBffOXTtwE0a9MsxHClwBLqCEnyYV+eSNB/seL/UqZqKRjs6q6BA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"dc2fe8dae40f305379fb3c30535f5325c961a9c1d9af32162c4ae534ce9f8b43","last_reissued_at":"2026-05-18T00:43:50.308481Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:43:50.308481Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Mass Loss Rates from Coronal Mass Ejections: A Predictive Theoretical Model for Solar-Type Stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Steven R. Cranmer (CU Boulder)","submitted_at":"2017-04-21T19:31:30Z","abstract_excerpt":"Coronal mass ejections (CMEs) are eruptive events that cause a solar-type star to shed mass and magnetic flux. CMEs tend to occur together with flares, radio storms, and bursts of energetic particles. On the Sun, CME-related mass loss is roughly an order of magnitude less intense than that of the background solar wind. However, on other types of stars, CMEs have been proposed to carry away much more mass and energy than the time-steady wind. Earlier papers have used observed correlations between solar CMEs and flare energies, in combination with stellar flare observations, to estimate stellar "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1704.06689","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":"1704.06689","created_at":"2026-05-18T00:43:50.308580+00:00"},{"alias_kind":"arxiv_version","alias_value":"1704.06689v1","created_at":"2026-05-18T00:43:50.308580+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1704.06689","created_at":"2026-05-18T00:43:50.308580+00:00"},{"alias_kind":"pith_short_12","alias_value":"3QX6RWXEB4YF","created_at":"2026-05-18T12:30:58.224056+00:00"},{"alias_kind":"pith_short_16","alias_value":"3QX6RWXEB4YFG6P3","created_at":"2026-05-18T12:30:58.224056+00:00"},{"alias_kind":"pith_short_8","alias_value":"3QX6RWXE","created_at":"2026-05-18T12:30:58.224056+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.04196","citing_title":"Probing Flare-Associated Eruptions on AB Doradus via X-ray Absorption Variations","ref_index":49,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/3QX6RWXEB4YFG6P3HQYFGX2TEX","json":"https://pith.science/pith/3QX6RWXEB4YFG6P3HQYFGX2TEX.json","graph_json":"https://pith.science/api/pith-number/3QX6RWXEB4YFG6P3HQYFGX2TEX/graph.json","events_json":"https://pith.science/api/pith-number/3QX6RWXEB4YFG6P3HQYFGX2TEX/events.json","paper":"https://pith.science/paper/3QX6RWXE"},"agent_actions":{"view_html":"https://pith.science/pith/3QX6RWXEB4YFG6P3HQYFGX2TEX","download_json":"https://pith.science/pith/3QX6RWXEB4YFG6P3HQYFGX2TEX.json","view_paper":"https://pith.science/paper/3QX6RWXE","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1704.06689&json=true","fetch_graph":"https://pith.science/api/pith-number/3QX6RWXEB4YFG6P3HQYFGX2TEX/graph.json","fetch_events":"https://pith.science/api/pith-number/3QX6RWXEB4YFG6P3HQYFGX2TEX/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/3QX6RWXEB4YFG6P3HQYFGX2TEX/action/timestamp_anchor","attest_storage":"https://pith.science/pith/3QX6RWXEB4YFG6P3HQYFGX2TEX/action/storage_attestation","attest_author":"https://pith.science/pith/3QX6RWXEB4YFG6P3HQYFGX2TEX/action/author_attestation","sign_citation":"https://pith.science/pith/3QX6RWXEB4YFG6P3HQYFGX2TEX/action/citation_signature","submit_replication":"https://pith.science/pith/3QX6RWXEB4YFG6P3HQYFGX2TEX/action/replication_record"}},"created_at":"2026-05-18T00:43:50.308580+00:00","updated_at":"2026-05-18T00:43:50.308580+00:00"}