{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:A7RPW6BTWQ2PWACNHV6EY7W2GG","short_pith_number":"pith:A7RPW6BT","schema_version":"1.0","canonical_sha256":"07e2fb7833b434fb004d3d7c4c7eda31b2fbaa3fc6f7676ca7adfed84ce1f79a","source":{"kind":"arxiv","id":"1903.01686","version":1},"attestation_state":"computed","paper":{"title":"X-ray and Optical Monitoring of State Transitions in MAXI J1820+070","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Hitoshi Negoro, Katsuhiro L. Murata, Megumi Shidatsu, Nobuyuki Kawai, Ryo Adachi, Satoshi Nakahira, Yoshihiro Ueda","submitted_at":"2019-03-05T06:00:34Z","abstract_excerpt":"We report results from the X-ray and optical monitoring of the black hole candidate MAXI J1820+070 (=ASSASN-18ey) over the entire period of its outburst from March to October 2018.In this outburst, the source exhibited two sets of `fast rise and slow decay'-type long-term flux variations. We found that the 1--100 keV luminosities at two peaks were almost the same, although a significant spectral softening was only seen in the second flux rise. This confirms that the state transition from the low/hard state to the high/soft state is not determined by the mass accretion rate alone. The X-ray spe"},"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":"1903.01686","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2019-03-05T06:00:34Z","cross_cats_sorted":[],"title_canon_sha256":"0f6a65ca7583264e5e95d96a004611ca38735cbcede6298cfc1025dd290b1012","abstract_canon_sha256":"982b3a97d4b1d52b4868e6a89921264a1128e4bb4d9891252c693403ed3e5618"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:48:30.126485Z","signature_b64":"wgw9XRKeBK3VsXozZmVfaP6xpx2jEjt/eL5As+9LZGKm+zBl/oL+3M/Hb4Iay5kdhIIu1EoysySYroYax4V5Bg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"07e2fb7833b434fb004d3d7c4c7eda31b2fbaa3fc6f7676ca7adfed84ce1f79a","last_reissued_at":"2026-05-17T23:48:30.125815Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:48:30.125815Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"X-ray and Optical Monitoring of State Transitions in MAXI J1820+070","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Hitoshi Negoro, Katsuhiro L. Murata, Megumi Shidatsu, Nobuyuki Kawai, Ryo Adachi, Satoshi Nakahira, Yoshihiro Ueda","submitted_at":"2019-03-05T06:00:34Z","abstract_excerpt":"We report results from the X-ray and optical monitoring of the black hole candidate MAXI J1820+070 (=ASSASN-18ey) over the entire period of its outburst from March to October 2018.In this outburst, the source exhibited two sets of `fast rise and slow decay'-type long-term flux variations. We found that the 1--100 keV luminosities at two peaks were almost the same, although a significant spectral softening was only seen in the second flux rise. This confirms that the state transition from the low/hard state to the high/soft state is not determined by the mass accretion rate alone. The X-ray spe"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1903.01686","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":"1903.01686","created_at":"2026-05-17T23:48:30.125939+00:00"},{"alias_kind":"arxiv_version","alias_value":"1903.01686v1","created_at":"2026-05-17T23:48:30.125939+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1903.01686","created_at":"2026-05-17T23:48:30.125939+00:00"},{"alias_kind":"pith_short_12","alias_value":"A7RPW6BTWQ2P","created_at":"2026-05-18T12:33:12.712433+00:00"},{"alias_kind":"pith_short_16","alias_value":"A7RPW6BTWQ2PWACN","created_at":"2026-05-18T12:33:12.712433+00:00"},{"alias_kind":"pith_short_8","alias_value":"A7RPW6BT","created_at":"2026-05-18T12:33:12.712433+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.19473","citing_title":"Radio-X-ray Time Lags in GX 339-4: Probing Magnetic Field Transport in Black Hole Accretion","ref_index":251,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/A7RPW6BTWQ2PWACNHV6EY7W2GG","json":"https://pith.science/pith/A7RPW6BTWQ2PWACNHV6EY7W2GG.json","graph_json":"https://pith.science/api/pith-number/A7RPW6BTWQ2PWACNHV6EY7W2GG/graph.json","events_json":"https://pith.science/api/pith-number/A7RPW6BTWQ2PWACNHV6EY7W2GG/events.json","paper":"https://pith.science/paper/A7RPW6BT"},"agent_actions":{"view_html":"https://pith.science/pith/A7RPW6BTWQ2PWACNHV6EY7W2GG","download_json":"https://pith.science/pith/A7RPW6BTWQ2PWACNHV6EY7W2GG.json","view_paper":"https://pith.science/paper/A7RPW6BT","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1903.01686&json=true","fetch_graph":"https://pith.science/api/pith-number/A7RPW6BTWQ2PWACNHV6EY7W2GG/graph.json","fetch_events":"https://pith.science/api/pith-number/A7RPW6BTWQ2PWACNHV6EY7W2GG/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/A7RPW6BTWQ2PWACNHV6EY7W2GG/action/timestamp_anchor","attest_storage":"https://pith.science/pith/A7RPW6BTWQ2PWACNHV6EY7W2GG/action/storage_attestation","attest_author":"https://pith.science/pith/A7RPW6BTWQ2PWACNHV6EY7W2GG/action/author_attestation","sign_citation":"https://pith.science/pith/A7RPW6BTWQ2PWACNHV6EY7W2GG/action/citation_signature","submit_replication":"https://pith.science/pith/A7RPW6BTWQ2PWACNHV6EY7W2GG/action/replication_record"}},"created_at":"2026-05-17T23:48:30.125939+00:00","updated_at":"2026-05-17T23:48:30.125939+00:00"}