{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:KYLDZBAMNHALBRJWP45RTN7LUO","short_pith_number":"pith:KYLDZBAM","schema_version":"1.0","canonical_sha256":"56163c840c69c0b0c5367f3b19b7eba3bcaf360f466ee71221ae4408c35e133d","source":{"kind":"arxiv","id":"2104.06141","version":3},"attestation_state":"computed","paper":{"title":"Implications of Feebly Interacting Dark Sector on Neutron Star Properties and Constraints from GW170817","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.HE","hep-th","nucl-th"],"primary_cat":"hep-ph","authors_text":"Atanu Guha, Debashree Sen","submitted_at":"2021-04-13T12:31:50Z","abstract_excerpt":"We investigate the effect of feeble interaction of dark matter (DM) with hadronic matter on the equation of state (EoS) and structural properties of neutron stars (NSs) in static conditions. For the purpose we adopt the effective chiral model for the hadronic sector and for the first time in the context of possible existence of DM inside NSs, we introduce DM-SM interaction through light new physics mediator. Moreover, the mass of DM fermion, the mediator and the coupling are adopted from the self-interaction constraint from Bullet cluster and from present day relic abundance. Within the consid"},"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":"2104.06141","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"hep-ph","submitted_at":"2021-04-13T12:31:50Z","cross_cats_sorted":["astro-ph.CO","astro-ph.HE","hep-th","nucl-th"],"title_canon_sha256":"d8c5a593701034a092849c1c0c528d6adb1b542d97224956d980f898365f9e6f","abstract_canon_sha256":"c1439ee0b69a1873c047f8053fbebb8ad7e6f8a3b281185a99077a2d44635df3"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T02:46:45.498105Z","signature_b64":"zvWL2JUFklETVDVd/1rMBl/kw0tEg5DBWPG9/HNriJswy0lu7eggaPmNzgV2bXMZMV9ZOkr7fWhHJjsatlrmAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"56163c840c69c0b0c5367f3b19b7eba3bcaf360f466ee71221ae4408c35e133d","last_reissued_at":"2026-07-05T02:46:45.497585Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T02:46:45.497585Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Implications of Feebly Interacting Dark Sector on Neutron Star Properties and Constraints from GW170817","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.HE","hep-th","nucl-th"],"primary_cat":"hep-ph","authors_text":"Atanu Guha, Debashree Sen","submitted_at":"2021-04-13T12:31:50Z","abstract_excerpt":"We investigate the effect of feeble interaction of dark matter (DM) with hadronic matter on the equation of state (EoS) and structural properties of neutron stars (NSs) in static conditions. For the purpose we adopt the effective chiral model for the hadronic sector and for the first time in the context of possible existence of DM inside NSs, we introduce DM-SM interaction through light new physics mediator. Moreover, the mass of DM fermion, the mediator and the coupling are adopted from the self-interaction constraint from Bullet cluster and from present day relic abundance. Within the consid"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2104.06141","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/2104.06141/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":"2104.06141","created_at":"2026-07-05T02:46:45.497642+00:00"},{"alias_kind":"arxiv_version","alias_value":"2104.06141v3","created_at":"2026-07-05T02:46:45.497642+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2104.06141","created_at":"2026-07-05T02:46:45.497642+00:00"},{"alias_kind":"pith_short_12","alias_value":"KYLDZBAMNHAL","created_at":"2026-07-05T02:46:45.497642+00:00"},{"alias_kind":"pith_short_16","alias_value":"KYLDZBAMNHALBRJW","created_at":"2026-07-05T02:46:45.497642+00:00"},{"alias_kind":"pith_short_8","alias_value":"KYLDZBAM","created_at":"2026-07-05T02:46:45.497642+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.23620","citing_title":"Observables and conformal properties of dark matter admixed isentropic neutron stars","ref_index":69,"is_internal_anchor":false},{"citing_arxiv_id":"2607.00888","citing_title":"A self-consistent single-fluid framework for neutron stars admixed with mirror dark matter","ref_index":37,"is_internal_anchor":false},{"citing_arxiv_id":"2503.19691","citing_title":"Strongly Interacting Dark Matter admixed Neutron Stars","ref_index":45,"is_internal_anchor":false},{"citing_arxiv_id":"2105.06979","citing_title":"The Radius of PSR J0740+6620 from NICER and XMM-Newton Data","ref_index":108,"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":53,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/KYLDZBAMNHALBRJWP45RTN7LUO","json":"https://pith.science/pith/KYLDZBAMNHALBRJWP45RTN7LUO.json","graph_json":"https://pith.science/api/pith-number/KYLDZBAMNHALBRJWP45RTN7LUO/graph.json","events_json":"https://pith.science/api/pith-number/KYLDZBAMNHALBRJWP45RTN7LUO/events.json","paper":"https://pith.science/paper/KYLDZBAM"},"agent_actions":{"view_html":"https://pith.science/pith/KYLDZBAMNHALBRJWP45RTN7LUO","download_json":"https://pith.science/pith/KYLDZBAMNHALBRJWP45RTN7LUO.json","view_paper":"https://pith.science/paper/KYLDZBAM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2104.06141&json=true","fetch_graph":"https://pith.science/api/pith-number/KYLDZBAMNHALBRJWP45RTN7LUO/graph.json","fetch_events":"https://pith.science/api/pith-number/KYLDZBAMNHALBRJWP45RTN7LUO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/KYLDZBAMNHALBRJWP45RTN7LUO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/KYLDZBAMNHALBRJWP45RTN7LUO/action/storage_attestation","attest_author":"https://pith.science/pith/KYLDZBAMNHALBRJWP45RTN7LUO/action/author_attestation","sign_citation":"https://pith.science/pith/KYLDZBAMNHALBRJWP45RTN7LUO/action/citation_signature","submit_replication":"https://pith.science/pith/KYLDZBAMNHALBRJWP45RTN7LUO/action/replication_record"}},"created_at":"2026-07-05T02:46:45.497642+00:00","updated_at":"2026-07-05T02:46:45.497642+00:00"}