{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2000:Y3TB4AVSFXFSEW6VOA7HC63LTW","short_pith_number":"pith:Y3TB4AVS","schema_version":"1.0","canonical_sha256":"c6e61e02b22dcb225bd5703e717b6b9dab79c77ab0fc054da0a4e199c1e1e030","source":{"kind":"arxiv","id":"astro-ph/0003308","version":4},"attestation_state":"computed","paper":{"title":"Fourier power spectra at high frequencies: a way to distinguish a neutron star from a black hole","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"1) ((1)-MPA, 2), Garching bei M\\\"unchen, Germany;(2)-Space Research Institute, Moscow, M.Revnivtsev (2, R.Sunyaev (1, Russia)","submitted_at":"2000-03-21T22:37:48Z","abstract_excerpt":"We analyzed the power density spectra of a sample of 9 neutron star and 9 black hole binaries in the low/hard spectral state. In the power density spectra of accreting neutron stars with a weak magnetic field a significant power is contained at frequencies close to one kHz. At the same time, most Galactic accreting black holes demonstrate a strong decline in the power spectra at the frequencies higher than 10--50 Hz. We propose to use this empirical fact as a method to distinguish the accreting neutron stars from black holes in X-ray transients. The X-ray transients that demonstrate significan"},"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/0003308","kind":"arxiv","version":4},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2000-03-21T22:37:48Z","cross_cats_sorted":[],"title_canon_sha256":"dc730a878efcdd866f096c66f37c06f1d79aa8c79d2387d59e17425a9d343d87","abstract_canon_sha256":"7b4e013a097c0c200a14a092f45ea6bc9d12c9d4005ee1d286f4a11075edb2e6"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:21:42.716728Z","signature_b64":"saTzMYXrnvYdVABXNJCT/gqVVvdfwTU4lq5z/Sp/h0dwuZKG4DhWulKfeLJieFW6w461zRF4pHTVFicwb8lyDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c6e61e02b22dcb225bd5703e717b6b9dab79c77ab0fc054da0a4e199c1e1e030","last_reissued_at":"2026-05-18T04:21:42.716151Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:21:42.716151Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Fourier power spectra at high frequencies: a way to distinguish a neutron star from a black hole","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"1) ((1)-MPA, 2), Garching bei M\\\"unchen, Germany;(2)-Space Research Institute, Moscow, M.Revnivtsev (2, R.Sunyaev (1, Russia)","submitted_at":"2000-03-21T22:37:48Z","abstract_excerpt":"We analyzed the power density spectra of a sample of 9 neutron star and 9 black hole binaries in the low/hard spectral state. In the power density spectra of accreting neutron stars with a weak magnetic field a significant power is contained at frequencies close to one kHz. At the same time, most Galactic accreting black holes demonstrate a strong decline in the power spectra at the frequencies higher than 10--50 Hz. We propose to use this empirical fact as a method to distinguish the accreting neutron stars from black holes in X-ray transients. The X-ray transients that demonstrate significan"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0003308","kind":"arxiv","version":4},"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":"astro-ph/0003308","created_at":"2026-05-18T04:21:42.716231+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0003308v4","created_at":"2026-05-18T04:21:42.716231+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0003308","created_at":"2026-05-18T04:21:42.716231+00:00"},{"alias_kind":"pith_short_12","alias_value":"Y3TB4AVSFXFS","created_at":"2026-05-18T12:25:50.254431+00:00"},{"alias_kind":"pith_short_16","alias_value":"Y3TB4AVSFXFSEW6V","created_at":"2026-05-18T12:25:50.254431+00:00"},{"alias_kind":"pith_short_8","alias_value":"Y3TB4AVS","created_at":"2026-05-18T12:25:50.254431+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/Y3TB4AVSFXFSEW6VOA7HC63LTW","json":"https://pith.science/pith/Y3TB4AVSFXFSEW6VOA7HC63LTW.json","graph_json":"https://pith.science/api/pith-number/Y3TB4AVSFXFSEW6VOA7HC63LTW/graph.json","events_json":"https://pith.science/api/pith-number/Y3TB4AVSFXFSEW6VOA7HC63LTW/events.json","paper":"https://pith.science/paper/Y3TB4AVS"},"agent_actions":{"view_html":"https://pith.science/pith/Y3TB4AVSFXFSEW6VOA7HC63LTW","download_json":"https://pith.science/pith/Y3TB4AVSFXFSEW6VOA7HC63LTW.json","view_paper":"https://pith.science/paper/Y3TB4AVS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0003308&json=true","fetch_graph":"https://pith.science/api/pith-number/Y3TB4AVSFXFSEW6VOA7HC63LTW/graph.json","fetch_events":"https://pith.science/api/pith-number/Y3TB4AVSFXFSEW6VOA7HC63LTW/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/Y3TB4AVSFXFSEW6VOA7HC63LTW/action/timestamp_anchor","attest_storage":"https://pith.science/pith/Y3TB4AVSFXFSEW6VOA7HC63LTW/action/storage_attestation","attest_author":"https://pith.science/pith/Y3TB4AVSFXFSEW6VOA7HC63LTW/action/author_attestation","sign_citation":"https://pith.science/pith/Y3TB4AVSFXFSEW6VOA7HC63LTW/action/citation_signature","submit_replication":"https://pith.science/pith/Y3TB4AVSFXFSEW6VOA7HC63LTW/action/replication_record"}},"created_at":"2026-05-18T04:21:42.716231+00:00","updated_at":"2026-05-18T04:21:42.716231+00:00"}