{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2005:RVVNVQAHOQ64J74NBUTK64ZVUT","short_pith_number":"pith:RVVNVQAH","schema_version":"1.0","canonical_sha256":"8d6adac007743dc4ff8d0d26af7335a4e1e1fcd889e2f22f03cbaeb318d49771","source":{"kind":"arxiv","id":"hep-th/0506069","version":3},"attestation_state":"computed","paper":{"title":"Transition of the dark energy equation of state in an interacting holographic dark energy model","license":"","headline":"","cross_cats":["astro-ph","gr-qc"],"primary_cat":"hep-th","authors_text":"Bin Wang, Elcio Abdalla, Yungui Gong","submitted_at":"2005-06-09T07:15:09Z","abstract_excerpt":"A model of holographic dark energy with an interaction with matter fields has been investigated. Choosing the future event horizon as an IR cutoff, we have shown that the ratio of energy densities can vary with time. With the interaction between the two different constituents of the universe, we observed the evolution of the universe, from early deceleration to late time acceleration. In addition, we have found that such an interacting dark energy model can accommodate a transition of the dark energy from a normal state where $w_D>-1$ to $w_D<-1$ phantom regimes. Implications of interacting da"},"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":"hep-th/0506069","kind":"arxiv","version":3},"metadata":{"license":"","primary_cat":"hep-th","submitted_at":"2005-06-09T07:15:09Z","cross_cats_sorted":["astro-ph","gr-qc"],"title_canon_sha256":"412242ee2400ba9efbedaa63222ee4045574acec83cc42765067506a4d7d4b18","abstract_canon_sha256":"281b8c44ea82d593ee94283249d76ad3859f8921eb32d2590abc53fc69008b5a"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:56:13.054649Z","signature_b64":"Nv3N4PskGwTVn9BQYDSvwIuYH7bFpG9ZbaLa3jSFSsxgY8sHS7ufb8zG6OpgR5wyQuuV9Mw7SVhXgQhVRJJFAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8d6adac007743dc4ff8d0d26af7335a4e1e1fcd889e2f22f03cbaeb318d49771","last_reissued_at":"2026-07-04T16:56:13.054281Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:56:13.054281Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Transition of the dark energy equation of state in an interacting holographic dark energy model","license":"","headline":"","cross_cats":["astro-ph","gr-qc"],"primary_cat":"hep-th","authors_text":"Bin Wang, Elcio Abdalla, Yungui Gong","submitted_at":"2005-06-09T07:15:09Z","abstract_excerpt":"A model of holographic dark energy with an interaction with matter fields has been investigated. Choosing the future event horizon as an IR cutoff, we have shown that the ratio of energy densities can vary with time. With the interaction between the two different constituents of the universe, we observed the evolution of the universe, from early deceleration to late time acceleration. In addition, we have found that such an interacting dark energy model can accommodate a transition of the dark energy from a normal state where $w_D>-1$ to $w_D<-1$ phantom regimes. Implications of interacting da"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"hep-th/0506069","kind":"arxiv","version":3},"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/hep-th/0506069/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":"hep-th/0506069","created_at":"2026-07-04T16:56:13.054345+00:00"},{"alias_kind":"arxiv_version","alias_value":"hep-th/0506069v3","created_at":"2026-07-04T16:56:13.054345+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.hep-th/0506069","created_at":"2026-07-04T16:56:13.054345+00:00"},{"alias_kind":"pith_short_12","alias_value":"RVVNVQAHOQ64","created_at":"2026-07-04T16:56:13.054345+00:00"},{"alias_kind":"pith_short_16","alias_value":"RVVNVQAHOQ64J74N","created_at":"2026-07-04T16:56:13.054345+00:00"},{"alias_kind":"pith_short_8","alias_value":"RVVNVQAH","created_at":"2026-07-04T16:56:13.054345+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":5,"sample":[{"citing_arxiv_id":"2606.05539","citing_title":"Dissipative Cosmology and the Nature of Dark Energy: Insights from Bulk Viscosity with DESI DR2 observations","ref_index":59,"is_internal_anchor":true},{"citing_arxiv_id":"2606.01360","citing_title":"A short review on Quintom dark energy theory","ref_index":112,"is_internal_anchor":true},{"citing_arxiv_id":"2605.20060","citing_title":"Interacting Dark Sector field theory with phantom crossing","ref_index":7,"is_internal_anchor":true},{"citing_arxiv_id":"2505.24732","citing_title":"The Quintom theory of dark energy after DESI DR2","ref_index":205,"is_internal_anchor":true},{"citing_arxiv_id":"2511.09467","citing_title":"Revisiting the Hubble tension problem in the framework of holographic dark energy","ref_index":80,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/RVVNVQAHOQ64J74NBUTK64ZVUT","json":"https://pith.science/pith/RVVNVQAHOQ64J74NBUTK64ZVUT.json","graph_json":"https://pith.science/api/pith-number/RVVNVQAHOQ64J74NBUTK64ZVUT/graph.json","events_json":"https://pith.science/api/pith-number/RVVNVQAHOQ64J74NBUTK64ZVUT/events.json","paper":"https://pith.science/paper/RVVNVQAH"},"agent_actions":{"view_html":"https://pith.science/pith/RVVNVQAHOQ64J74NBUTK64ZVUT","download_json":"https://pith.science/pith/RVVNVQAHOQ64J74NBUTK64ZVUT.json","view_paper":"https://pith.science/paper/RVVNVQAH","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=hep-th/0506069&json=true","fetch_graph":"https://pith.science/api/pith-number/RVVNVQAHOQ64J74NBUTK64ZVUT/graph.json","fetch_events":"https://pith.science/api/pith-number/RVVNVQAHOQ64J74NBUTK64ZVUT/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/RVVNVQAHOQ64J74NBUTK64ZVUT/action/timestamp_anchor","attest_storage":"https://pith.science/pith/RVVNVQAHOQ64J74NBUTK64ZVUT/action/storage_attestation","attest_author":"https://pith.science/pith/RVVNVQAHOQ64J74NBUTK64ZVUT/action/author_attestation","sign_citation":"https://pith.science/pith/RVVNVQAHOQ64J74NBUTK64ZVUT/action/citation_signature","submit_replication":"https://pith.science/pith/RVVNVQAHOQ64J74NBUTK64ZVUT/action/replication_record"}},"created_at":"2026-07-04T16:56:13.054345+00:00","updated_at":"2026-07-04T16:56:13.054345+00:00"}