{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2000:ZE7WC7U6P5BN32OCH6RGFFFCWX","short_pith_number":"pith:ZE7WC7U6","schema_version":"1.0","canonical_sha256":"c93f617e9e7f42dde9c23fa26294a2b5e8abd5b56ff1835390358e12bc9f20b0","source":{"kind":"arxiv","id":"astro-ph/0006024","version":2},"attestation_state":"computed","paper":{"title":"A Further Analysis of a Cosmological Model of Quintessence and Scalar Dark Matter","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"L. A. Urena-Lopez (CINVESTAV), T. Matos","submitted_at":"2000-06-01T17:28:46Z","abstract_excerpt":"We present the complete solution to a 95% scalar field cosmological model in which the dark matter is modeled by a scalar field $\\Phi$ with the scalar potential $V(\\Phi)=V_{o}[ \\cosh {(\\lambda \\sqrt{\\kappa_{o}}\\Phi)}-1]$ and the dark energy is modeled by a scalar field $\\Psi$, endowed with the scalar potential $\\tilde{V}(\\Psi)=\\tilde{V_{o}}[ \\sinh {(\\alpha \\sqrt{\\kappa_{o}}\\Psi)}] ^{\\beta}$. This model has only two free parameters, $\\lambda$ and the equation of state $\\omega_{\\Psi}$. With these potentials, the fine tuning and the cosmic coincidence problems are ameliorated for both dark matter"},"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/0006024","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2000-06-01T17:28:46Z","cross_cats_sorted":[],"title_canon_sha256":"0e40810d52ff13973c964d718fea52c35799ffa1a532717d45c5e7b135b0091d","abstract_canon_sha256":"55be27d1794a3f08c8a860f7ab69a6dc3e70663e69fe1487095ef9bcc6430837"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:16:45.345576Z","signature_b64":"XcmB4KcdYWiOvewHJgiHMe9v8zDWfuMcH/8w9RqDzt4qSVe/9G3w9+pU+NHSEKhkyOoHThdw8n3lk2aQC9jnDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c93f617e9e7f42dde9c23fa26294a2b5e8abd5b56ff1835390358e12bc9f20b0","last_reissued_at":"2026-07-04T16:16:45.345124Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:16:45.345124Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A Further Analysis of a Cosmological Model of Quintessence and Scalar Dark Matter","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"L. A. Urena-Lopez (CINVESTAV), T. Matos","submitted_at":"2000-06-01T17:28:46Z","abstract_excerpt":"We present the complete solution to a 95% scalar field cosmological model in which the dark matter is modeled by a scalar field $\\Phi$ with the scalar potential $V(\\Phi)=V_{o}[ \\cosh {(\\lambda \\sqrt{\\kappa_{o}}\\Phi)}-1]$ and the dark energy is modeled by a scalar field $\\Psi$, endowed with the scalar potential $\\tilde{V}(\\Psi)=\\tilde{V_{o}}[ \\sinh {(\\alpha \\sqrt{\\kappa_{o}}\\Psi)}] ^{\\beta}$. This model has only two free parameters, $\\lambda$ and the equation of state $\\omega_{\\Psi}$. With these potentials, the fine tuning and the cosmic coincidence problems are ameliorated for both dark matter"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0006024","kind":"arxiv","version":2},"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/0006024/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/0006024","created_at":"2026-07-04T16:16:45.345194+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0006024v2","created_at":"2026-07-04T16:16:45.345194+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0006024","created_at":"2026-07-04T16:16:45.345194+00:00"},{"alias_kind":"pith_short_12","alias_value":"ZE7WC7U6P5BN","created_at":"2026-07-04T16:16:45.345194+00:00"},{"alias_kind":"pith_short_16","alias_value":"ZE7WC7U6P5BN32OC","created_at":"2026-07-04T16:16:45.345194+00:00"},{"alias_kind":"pith_short_8","alias_value":"ZE7WC7U6","created_at":"2026-07-04T16:16:45.345194+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2605.27529","citing_title":"Existence of nonrelativistic $\\ell$- and multi-$\\ell$-boson stars and their radial stability","ref_index":5,"is_internal_anchor":true},{"citing_arxiv_id":"2507.05207","citing_title":"Interacting Scalar Fields as Dark Energy and Dark Matter in Einstein scalar Gauss Bonnet Gravity","ref_index":94,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ZE7WC7U6P5BN32OCH6RGFFFCWX","json":"https://pith.science/pith/ZE7WC7U6P5BN32OCH6RGFFFCWX.json","graph_json":"https://pith.science/api/pith-number/ZE7WC7U6P5BN32OCH6RGFFFCWX/graph.json","events_json":"https://pith.science/api/pith-number/ZE7WC7U6P5BN32OCH6RGFFFCWX/events.json","paper":"https://pith.science/paper/ZE7WC7U6"},"agent_actions":{"view_html":"https://pith.science/pith/ZE7WC7U6P5BN32OCH6RGFFFCWX","download_json":"https://pith.science/pith/ZE7WC7U6P5BN32OCH6RGFFFCWX.json","view_paper":"https://pith.science/paper/ZE7WC7U6","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0006024&json=true","fetch_graph":"https://pith.science/api/pith-number/ZE7WC7U6P5BN32OCH6RGFFFCWX/graph.json","fetch_events":"https://pith.science/api/pith-number/ZE7WC7U6P5BN32OCH6RGFFFCWX/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ZE7WC7U6P5BN32OCH6RGFFFCWX/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ZE7WC7U6P5BN32OCH6RGFFFCWX/action/storage_attestation","attest_author":"https://pith.science/pith/ZE7WC7U6P5BN32OCH6RGFFFCWX/action/author_attestation","sign_citation":"https://pith.science/pith/ZE7WC7U6P5BN32OCH6RGFFFCWX/action/citation_signature","submit_replication":"https://pith.science/pith/ZE7WC7U6P5BN32OCH6RGFFFCWX/action/replication_record"}},"created_at":"2026-07-04T16:16:45.345194+00:00","updated_at":"2026-07-04T16:16:45.345194+00:00"}