{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2005:5IC5WRV7TFMGY5SZQ2QSWGIUM5","short_pith_number":"pith:5IC5WRV7","schema_version":"1.0","canonical_sha256":"ea05db46bf99586c765986a12b191467749fe6b48d5f9128849eb21dfc73a461","source":{"kind":"arxiv","id":"astro-ph/0503361","version":1},"attestation_state":"computed","paper":{"title":"A Computational Guide to Physics of Eclipsing Binaries. Paper I. Demonstrations and Perspectives","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Prsa, T. Zwitter","submitted_at":"2005-03-16T18:11:53Z","abstract_excerpt":"PHOEBE (PHysics Of Eclipsing BinariEs) is a modeling package for eclipsing binary stars, built on top of the widely used WD program (Wilson & Devinney 1971). This introductory paper overviews most important scientific extensions (incorporating observational spectra of eclipsing binaries into the solution-seeking process, extracting individual temperatures from observed color indices, main-sequence constraining and proper treatment of the reddening), numerical innovations (suggested improvements to WD's Differential Corrections method, the new Nelder & Mead's downhill Simplex method) and techni"},"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/0503361","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2005-03-16T18:11:53Z","cross_cats_sorted":[],"title_canon_sha256":"25f9a1437e13512dc01a1b1f84a45213062b642e040428d4a80a8e6d54a7fdf1","abstract_canon_sha256":"44de14af27ac33984db4a561f70f0b5d23b4a84cdb0fc22260bfe17eda1f4c93"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:51:01.011341Z","signature_b64":"5gl2j5g0aLVLTEjCsAKbNDQJrZ4XatYVKDU4XDDlXIKMLdxZ7rTLEAToZtRcSjCpNwqk+01fz0ytryM+d4/8AQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ea05db46bf99586c765986a12b191467749fe6b48d5f9128849eb21dfc73a461","last_reissued_at":"2026-07-04T16:51:01.010928Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:51:01.010928Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A Computational Guide to Physics of Eclipsing Binaries. Paper I. Demonstrations and Perspectives","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Prsa, T. Zwitter","submitted_at":"2005-03-16T18:11:53Z","abstract_excerpt":"PHOEBE (PHysics Of Eclipsing BinariEs) is a modeling package for eclipsing binary stars, built on top of the widely used WD program (Wilson & Devinney 1971). This introductory paper overviews most important scientific extensions (incorporating observational spectra of eclipsing binaries into the solution-seeking process, extracting individual temperatures from observed color indices, main-sequence constraining and proper treatment of the reddening), numerical innovations (suggested improvements to WD's Differential Corrections method, the new Nelder & Mead's downhill Simplex method) and techni"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0503361","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/0503361/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/0503361","created_at":"2026-07-04T16:51:01.010989+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0503361v1","created_at":"2026-07-04T16:51:01.010989+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0503361","created_at":"2026-07-04T16:51:01.010989+00:00"},{"alias_kind":"pith_short_12","alias_value":"5IC5WRV7TFMG","created_at":"2026-07-04T16:51:01.010989+00:00"},{"alias_kind":"pith_short_16","alias_value":"5IC5WRV7TFMGY5SZ","created_at":"2026-07-04T16:51:01.010989+00:00"},{"alias_kind":"pith_short_8","alias_value":"5IC5WRV7","created_at":"2026-07-04T16:51:01.010989+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2607.05977","citing_title":"TESS light curves and surface activity in two low-mass eclipsing binaries: NSVS 01031772 and 2MASS J04100497+2931023","ref_index":19,"is_internal_anchor":true},{"citing_arxiv_id":"2606.30748","citing_title":"The forgotten bright star: Theta Eridani as a millenary stellar transient observed by Hipparchus, Ptolemy and al-Sufi","ref_index":36,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/5IC5WRV7TFMGY5SZQ2QSWGIUM5","json":"https://pith.science/pith/5IC5WRV7TFMGY5SZQ2QSWGIUM5.json","graph_json":"https://pith.science/api/pith-number/5IC5WRV7TFMGY5SZQ2QSWGIUM5/graph.json","events_json":"https://pith.science/api/pith-number/5IC5WRV7TFMGY5SZQ2QSWGIUM5/events.json","paper":"https://pith.science/paper/5IC5WRV7"},"agent_actions":{"view_html":"https://pith.science/pith/5IC5WRV7TFMGY5SZQ2QSWGIUM5","download_json":"https://pith.science/pith/5IC5WRV7TFMGY5SZQ2QSWGIUM5.json","view_paper":"https://pith.science/paper/5IC5WRV7","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0503361&json=true","fetch_graph":"https://pith.science/api/pith-number/5IC5WRV7TFMGY5SZQ2QSWGIUM5/graph.json","fetch_events":"https://pith.science/api/pith-number/5IC5WRV7TFMGY5SZQ2QSWGIUM5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/5IC5WRV7TFMGY5SZQ2QSWGIUM5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/5IC5WRV7TFMGY5SZQ2QSWGIUM5/action/storage_attestation","attest_author":"https://pith.science/pith/5IC5WRV7TFMGY5SZQ2QSWGIUM5/action/author_attestation","sign_citation":"https://pith.science/pith/5IC5WRV7TFMGY5SZQ2QSWGIUM5/action/citation_signature","submit_replication":"https://pith.science/pith/5IC5WRV7TFMGY5SZQ2QSWGIUM5/action/replication_record"}},"created_at":"2026-07-04T16:51:01.010989+00:00","updated_at":"2026-07-04T16:51:01.010989+00:00"}