{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:STYWCGMGT7BAZ6MGD4ZK7YBRUP","short_pith_number":"pith:STYWCGMG","schema_version":"1.0","canonical_sha256":"94f16119869fc20cf9861f32afe031a3c54df9e66fc3c873d79e3ef7e6a4de0b","source":{"kind":"arxiv","id":"1502.03550","version":1},"attestation_state":"computed","paper":{"title":"Affleck-Dine baryogenesis after D-term inflation and solutions to the baryon-DM coincidence problem","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"hep-ph","authors_text":"Masahiro Kawasaki, Masaki Yamada","submitted_at":"2015-02-12T06:08:01Z","abstract_excerpt":"We investigate the Affleck-Dine baryogenesis after D-term inflation with a positive Hubble-induced mass term for a B-L flat direction. It stays at a large field value during D-term inflation, and just after inflation ends it starts to oscillate around the origin of the potential due to the positive Hubble-induced mass term. The phase direction is kicked by higher-dimensional Kahler potentials to generate the B-L asymmetry. The scenario predicts nonzero baryonic isocurvature perturbations, which would be detected by future observations of CMB fluctuations. We also provide a D-term inflation mod"},"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":"1502.03550","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"hep-ph","submitted_at":"2015-02-12T06:08:01Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"54ebb098b4723ff913e4ce75d7872295243a11d503763fba97ec7d5f3a799f79","abstract_canon_sha256":"37fa32bdd3120d013e1929b74e666d6c987890646e5cc9562c1d2befb5c5f0e5"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:18:42.666265Z","signature_b64":"cOWrplFSuy2icTJtpd7ky403Uyk8IOv+wHxWCObTYg4mURUPi8QobQmvyCZCXpmvVB5rmgFLsVKW0ro60JBiBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"94f16119869fc20cf9861f32afe031a3c54df9e66fc3c873d79e3ef7e6a4de0b","last_reissued_at":"2026-05-18T02:18:42.665500Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:18:42.665500Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Affleck-Dine baryogenesis after D-term inflation and solutions to the baryon-DM coincidence problem","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"hep-ph","authors_text":"Masahiro Kawasaki, Masaki Yamada","submitted_at":"2015-02-12T06:08:01Z","abstract_excerpt":"We investigate the Affleck-Dine baryogenesis after D-term inflation with a positive Hubble-induced mass term for a B-L flat direction. It stays at a large field value during D-term inflation, and just after inflation ends it starts to oscillate around the origin of the potential due to the positive Hubble-induced mass term. The phase direction is kicked by higher-dimensional Kahler potentials to generate the B-L asymmetry. The scenario predicts nonzero baryonic isocurvature perturbations, which would be detected by future observations of CMB fluctuations. We also provide a D-term inflation mod"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1502.03550","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":""},"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":"1502.03550","created_at":"2026-05-18T02:18:42.665637+00:00"},{"alias_kind":"arxiv_version","alias_value":"1502.03550v1","created_at":"2026-05-18T02:18:42.665637+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1502.03550","created_at":"2026-05-18T02:18:42.665637+00:00"},{"alias_kind":"pith_short_12","alias_value":"STYWCGMGT7BA","created_at":"2026-05-18T12:29:42.218222+00:00"},{"alias_kind":"pith_short_16","alias_value":"STYWCGMGT7BAZ6MG","created_at":"2026-05-18T12:29:42.218222+00:00"},{"alias_kind":"pith_short_8","alias_value":"STYWCGMG","created_at":"2026-05-18T12:29:42.218222+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.05309","citing_title":"Parametric Resonance of Higgsed Vector Dark Matter: Inflationary Initial Conditions and Sourced Displacements","ref_index":27,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/STYWCGMGT7BAZ6MGD4ZK7YBRUP","json":"https://pith.science/pith/STYWCGMGT7BAZ6MGD4ZK7YBRUP.json","graph_json":"https://pith.science/api/pith-number/STYWCGMGT7BAZ6MGD4ZK7YBRUP/graph.json","events_json":"https://pith.science/api/pith-number/STYWCGMGT7BAZ6MGD4ZK7YBRUP/events.json","paper":"https://pith.science/paper/STYWCGMG"},"agent_actions":{"view_html":"https://pith.science/pith/STYWCGMGT7BAZ6MGD4ZK7YBRUP","download_json":"https://pith.science/pith/STYWCGMGT7BAZ6MGD4ZK7YBRUP.json","view_paper":"https://pith.science/paper/STYWCGMG","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1502.03550&json=true","fetch_graph":"https://pith.science/api/pith-number/STYWCGMGT7BAZ6MGD4ZK7YBRUP/graph.json","fetch_events":"https://pith.science/api/pith-number/STYWCGMGT7BAZ6MGD4ZK7YBRUP/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/STYWCGMGT7BAZ6MGD4ZK7YBRUP/action/timestamp_anchor","attest_storage":"https://pith.science/pith/STYWCGMGT7BAZ6MGD4ZK7YBRUP/action/storage_attestation","attest_author":"https://pith.science/pith/STYWCGMGT7BAZ6MGD4ZK7YBRUP/action/author_attestation","sign_citation":"https://pith.science/pith/STYWCGMGT7BAZ6MGD4ZK7YBRUP/action/citation_signature","submit_replication":"https://pith.science/pith/STYWCGMGT7BAZ6MGD4ZK7YBRUP/action/replication_record"}},"created_at":"2026-05-18T02:18:42.665637+00:00","updated_at":"2026-05-18T02:18:42.665637+00:00"}