{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:PQ7VGEJRERPRVUJHB46DWEPYN5","short_pith_number":"pith:PQ7VGEJR","schema_version":"1.0","canonical_sha256":"7c3f531131245f1ad1270f3c3b11f86f66c2a4aabaf36bef43b5810be33706f7","source":{"kind":"arxiv","id":"2402.18696","version":1},"attestation_state":"computed","paper":{"title":"Exploring the distribution and impact of bosonic dark matter in neutron stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"Davood Rafiei Karkevandi, Mahboubeh Shahrbaf, Soroush Shakeri, Stefan Typel","submitted_at":"2024-02-28T20:24:26Z","abstract_excerpt":"The presence of dark matter (DM) within neutron stars (NSs) can be introduced by different accumulation scenarios in which DM and baryonic matter (BM) may interact only through the gravitational force. In this work, we consider asymmetric self-interacting bosonic DM which can reside as a dense core inside the NS or form an extended halo around it. It is seen that depending on the boson mass ($m_{\\chi}$), self-coupling constant ($\\lambda$) and DM fraction ($F_{\\chi}$), the maximum mass, radius and tidal deformability of NSs with DM admixture will be altered significantly. The impact of DM cause"},"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":"2402.18696","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2024-02-28T20:24:26Z","cross_cats_sorted":["nucl-th"],"title_canon_sha256":"e4a6fcbcf8e60e661ba8cc54e610638d0d3e76f60830fe6226aa787c265461e3","abstract_canon_sha256":"6542e19a3849f7f0763d7dc6e7a04ffc9ec92e08b234e6d84ab9d99941ee7631"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T07:51:40.611602Z","signature_b64":"d6BeMI0ctsc/BFYoZF4oYZvQYjU1/6O9tLJ7f/21ZjXIBAO5ZjpeN33ttFK5vcu3Qx1X29Ddti/mduJ9I8fbAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7c3f531131245f1ad1270f3c3b11f86f66c2a4aabaf36bef43b5810be33706f7","last_reissued_at":"2026-07-05T07:51:40.611137Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T07:51:40.611137Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Exploring the distribution and impact of bosonic dark matter in neutron stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"Davood Rafiei Karkevandi, Mahboubeh Shahrbaf, Soroush Shakeri, Stefan Typel","submitted_at":"2024-02-28T20:24:26Z","abstract_excerpt":"The presence of dark matter (DM) within neutron stars (NSs) can be introduced by different accumulation scenarios in which DM and baryonic matter (BM) may interact only through the gravitational force. In this work, we consider asymmetric self-interacting bosonic DM which can reside as a dense core inside the NS or form an extended halo around it. It is seen that depending on the boson mass ($m_{\\chi}$), self-coupling constant ($\\lambda$) and DM fraction ($F_{\\chi}$), the maximum mass, radius and tidal deformability of NSs with DM admixture will be altered significantly. The impact of DM cause"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2402.18696","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/2402.18696/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":"2402.18696","created_at":"2026-07-05T07:51:40.611197+00:00"},{"alias_kind":"arxiv_version","alias_value":"2402.18696v1","created_at":"2026-07-05T07:51:40.611197+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2402.18696","created_at":"2026-07-05T07:51:40.611197+00:00"},{"alias_kind":"pith_short_12","alias_value":"PQ7VGEJRERPR","created_at":"2026-07-05T07:51:40.611197+00:00"},{"alias_kind":"pith_short_16","alias_value":"PQ7VGEJRERPRVUJH","created_at":"2026-07-05T07:51:40.611197+00:00"},{"alias_kind":"pith_short_8","alias_value":"PQ7VGEJR","created_at":"2026-07-05T07:51:40.611197+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.27456","citing_title":"The crust of dark-matter admixed neutron stars: bulk properties and torsional oscillations","ref_index":69,"is_internal_anchor":false},{"citing_arxiv_id":"2503.19691","citing_title":"Strongly Interacting Dark Matter admixed Neutron Stars","ref_index":56,"is_internal_anchor":false},{"citing_arxiv_id":"2511.07567","citing_title":"Dark Matter Heating in Evolving Proto-Neutron Stars: A Two-Fluid Approach","ref_index":38,"is_internal_anchor":false},{"citing_arxiv_id":"2605.14447","citing_title":"Bayesian analysis of density profile of light dark matter elucidating the properties of dark matter admixed neutron stars in the presence of hyperons","ref_index":74,"is_internal_anchor":false},{"citing_arxiv_id":"2604.04560","citing_title":"Neutron star with dark matter using vector portal","ref_index":16,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/PQ7VGEJRERPRVUJHB46DWEPYN5","json":"https://pith.science/pith/PQ7VGEJRERPRVUJHB46DWEPYN5.json","graph_json":"https://pith.science/api/pith-number/PQ7VGEJRERPRVUJHB46DWEPYN5/graph.json","events_json":"https://pith.science/api/pith-number/PQ7VGEJRERPRVUJHB46DWEPYN5/events.json","paper":"https://pith.science/paper/PQ7VGEJR"},"agent_actions":{"view_html":"https://pith.science/pith/PQ7VGEJRERPRVUJHB46DWEPYN5","download_json":"https://pith.science/pith/PQ7VGEJRERPRVUJHB46DWEPYN5.json","view_paper":"https://pith.science/paper/PQ7VGEJR","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2402.18696&json=true","fetch_graph":"https://pith.science/api/pith-number/PQ7VGEJRERPRVUJHB46DWEPYN5/graph.json","fetch_events":"https://pith.science/api/pith-number/PQ7VGEJRERPRVUJHB46DWEPYN5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PQ7VGEJRERPRVUJHB46DWEPYN5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PQ7VGEJRERPRVUJHB46DWEPYN5/action/storage_attestation","attest_author":"https://pith.science/pith/PQ7VGEJRERPRVUJHB46DWEPYN5/action/author_attestation","sign_citation":"https://pith.science/pith/PQ7VGEJRERPRVUJHB46DWEPYN5/action/citation_signature","submit_replication":"https://pith.science/pith/PQ7VGEJRERPRVUJHB46DWEPYN5/action/replication_record"}},"created_at":"2026-07-05T07:51:40.611197+00:00","updated_at":"2026-07-05T07:51:40.611197+00:00"}