{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1997:QD3Q76224G3KEJ67YXR4X7SY5C","short_pith_number":"pith:QD3Q7622","schema_version":"1.0","canonical_sha256":"80f70ffb5ae1b6a227dfc5e3cbfe58e8ab5303ec2d8b664b9723e21d0b922df8","source":{"kind":"arxiv","id":"astro-ph/9702048","version":1},"attestation_state":"computed","paper":{"title":"An unstable central disk in the superluminal black-hole X-ray binary GRS 1915+105","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A.R. King, J. van Paradijs, M. Mendez, M. van der Klis, T. Belloni","submitted_at":"1997-02-05T09:42:14Z","abstract_excerpt":"We have analyzed the X-ray spectra of the microquasar GRS 1915+105, as observed with the PCA on the Rossi XTE, during periods of stable weak emission, outbursts and rapid flaring. We find that the complicated X-ray intensity curve of this source can be described by the rapid removal and replenishment of matter forming the inner part of an optically thick accretion disk, probably caused by a thermal-viscous instability analogous to that operating in dwarf novae, but here driven by the Lightman-Eardley instability. We find that the mass accretion rate in quiescence is 10^-6 solar masses per year"},"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":"astro-ph/9702048","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1997-02-05T09:42:14Z","cross_cats_sorted":[],"title_canon_sha256":"d33a9fdb6eed2cc2b6bed5adcb41575879755b0af603d3827ad4d09229a9fd1f","abstract_canon_sha256":"844d3facc2662a4ad94a865b97864a95000178e1b667c6ab1e479108f33d0c47"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:02:51.628097Z","signature_b64":"RwPFsZvBx1d8MAg3//zOUoTJm2MiFOEVLNMAfA1pSHMHAJbUWK4RWzz57wHZHU6NOfTIc/PSFCTwxB4Ehe6nCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"80f70ffb5ae1b6a227dfc5e3cbfe58e8ab5303ec2d8b664b9723e21d0b922df8","last_reissued_at":"2026-07-04T16:02:51.627759Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:02:51.627759Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"An unstable central disk in the superluminal black-hole X-ray binary GRS 1915+105","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A.R. King, J. van Paradijs, M. Mendez, M. van der Klis, T. Belloni","submitted_at":"1997-02-05T09:42:14Z","abstract_excerpt":"We have analyzed the X-ray spectra of the microquasar GRS 1915+105, as observed with the PCA on the Rossi XTE, during periods of stable weak emission, outbursts and rapid flaring. We find that the complicated X-ray intensity curve of this source can be described by the rapid removal and replenishment of matter forming the inner part of an optically thick accretion disk, probably caused by a thermal-viscous instability analogous to that operating in dwarf novae, but here driven by the Lightman-Eardley instability. We find that the mass accretion rate in quiescence is 10^-6 solar masses per year"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9702048","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/astro-ph/9702048/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":"astro-ph/9702048","created_at":"2026-07-04T16:02:51.627811+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9702048v1","created_at":"2026-07-04T16:02:51.627811+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9702048","created_at":"2026-07-04T16:02:51.627811+00:00"},{"alias_kind":"pith_short_12","alias_value":"QD3Q76224G3K","created_at":"2026-07-04T16:02:51.627811+00:00"},{"alias_kind":"pith_short_16","alias_value":"QD3Q76224G3KEJ67","created_at":"2026-07-04T16:02:51.627811+00:00"},{"alias_kind":"pith_short_8","alias_value":"QD3Q7622","created_at":"2026-07-04T16:02:51.627811+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2606.01823","citing_title":"A 0.03 Hz Radio Quasi-periodic Oscillation During the 2025 Flare of GRS 1915+105","ref_index":36,"is_internal_anchor":true},{"citing_arxiv_id":"2606.17976","citing_title":"An atypical X-ray variability component in the black hole candidate AT2019wey","ref_index":103,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/QD3Q76224G3KEJ67YXR4X7SY5C","json":"https://pith.science/pith/QD3Q76224G3KEJ67YXR4X7SY5C.json","graph_json":"https://pith.science/api/pith-number/QD3Q76224G3KEJ67YXR4X7SY5C/graph.json","events_json":"https://pith.science/api/pith-number/QD3Q76224G3KEJ67YXR4X7SY5C/events.json","paper":"https://pith.science/paper/QD3Q7622"},"agent_actions":{"view_html":"https://pith.science/pith/QD3Q76224G3KEJ67YXR4X7SY5C","download_json":"https://pith.science/pith/QD3Q76224G3KEJ67YXR4X7SY5C.json","view_paper":"https://pith.science/paper/QD3Q7622","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9702048&json=true","fetch_graph":"https://pith.science/api/pith-number/QD3Q76224G3KEJ67YXR4X7SY5C/graph.json","fetch_events":"https://pith.science/api/pith-number/QD3Q76224G3KEJ67YXR4X7SY5C/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/QD3Q76224G3KEJ67YXR4X7SY5C/action/timestamp_anchor","attest_storage":"https://pith.science/pith/QD3Q76224G3KEJ67YXR4X7SY5C/action/storage_attestation","attest_author":"https://pith.science/pith/QD3Q76224G3KEJ67YXR4X7SY5C/action/author_attestation","sign_citation":"https://pith.science/pith/QD3Q76224G3KEJ67YXR4X7SY5C/action/citation_signature","submit_replication":"https://pith.science/pith/QD3Q76224G3KEJ67YXR4X7SY5C/action/replication_record"}},"created_at":"2026-07-04T16:02:51.627811+00:00","updated_at":"2026-07-04T16:02:51.627811+00:00"}