{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:26B75WXZ7ZFIOHAPRDWX2VQIGM","short_pith_number":"pith:26B75WXZ","schema_version":"1.0","canonical_sha256":"d783fedaf9fe4a871c0f88ed7d5608333b25c559e3553d158a8e6821fab55892","source":{"kind":"arxiv","id":"2207.02433","version":1},"attestation_state":"computed","paper":{"title":"Tidal Deformability of Dark Matter Admixed Neutron Stars","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Kwing-Lam Leung, Lap-Ming Lin, Ming-chung Chu","submitted_at":"2022-07-06T04:41:31Z","abstract_excerpt":"The tidal properties of a neutron star are measurable in the gravitational waves emitted from inspiraling binary neutron stars, and they have been used to constrain the neutron star equation of state. In the same spirit, we study the dimensionless tidal deformability of dark matter admixed neutron stars. The tidal Love number is computed in a two-fluid framework. The dimensionless tidal Love number and dimensionless tidal deformability are computed for dark matter admixed stars with the dark matter modelled as ideal Fermi gas or self-interactive bosons. The dimensionless tidal deformability sh"},"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":"2207.02433","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2022-07-06T04:41:31Z","cross_cats_sorted":[],"title_canon_sha256":"4b6edd839318e4b5d55515018ab906f574a401b2f35802123bd0b36f9adf41ec","abstract_canon_sha256":"fef9739b1e8ff95d103885e1603b256c8d6f18599f35e68f244978cd1b77b85a"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:38:03.091123Z","signature_b64":"Ll+6l2qIw1VWeMtaxMbriBLhnOpiRLcmiAjsKUmVcMFychVmwhL/D7l26tYLqZH6TSzY0ckh0my1tACivZECAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d783fedaf9fe4a871c0f88ed7d5608333b25c559e3553d158a8e6821fab55892","last_reissued_at":"2026-07-05T04:38:03.090683Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:38:03.090683Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Tidal Deformability of Dark Matter Admixed Neutron Stars","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Kwing-Lam Leung, Lap-Ming Lin, Ming-chung Chu","submitted_at":"2022-07-06T04:41:31Z","abstract_excerpt":"The tidal properties of a neutron star are measurable in the gravitational waves emitted from inspiraling binary neutron stars, and they have been used to constrain the neutron star equation of state. In the same spirit, we study the dimensionless tidal deformability of dark matter admixed neutron stars. The tidal Love number is computed in a two-fluid framework. The dimensionless tidal Love number and dimensionless tidal deformability are computed for dark matter admixed stars with the dark matter modelled as ideal Fermi gas or self-interactive bosons. The dimensionless tidal deformability sh"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2207.02433","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/2207.02433/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":"2207.02433","created_at":"2026-07-05T04:38:03.090742+00:00"},{"alias_kind":"arxiv_version","alias_value":"2207.02433v1","created_at":"2026-07-05T04:38:03.090742+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2207.02433","created_at":"2026-07-05T04:38:03.090742+00:00"},{"alias_kind":"pith_short_12","alias_value":"26B75WXZ7ZFI","created_at":"2026-07-05T04:38:03.090742+00:00"},{"alias_kind":"pith_short_16","alias_value":"26B75WXZ7ZFIOHAP","created_at":"2026-07-05T04:38:03.090742+00:00"},{"alias_kind":"pith_short_8","alias_value":"26B75WXZ","created_at":"2026-07-05T04:38:03.090742+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":6,"is_internal_anchor":false},{"citing_arxiv_id":"2606.27456","citing_title":"The crust of dark-matter admixed neutron stars: bulk properties and torsional oscillations","ref_index":19,"is_internal_anchor":false},{"citing_arxiv_id":"2511.06489","citing_title":"Sub-GeV dark matter in neutron stars: halo morphologies and their suppression by vacuum-like pressure","ref_index":18,"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":54,"is_internal_anchor":false},{"citing_arxiv_id":"2605.10467","citing_title":"Axial Quasi-normal Modes of Admixed Neutron Stars","ref_index":37,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/26B75WXZ7ZFIOHAPRDWX2VQIGM","json":"https://pith.science/pith/26B75WXZ7ZFIOHAPRDWX2VQIGM.json","graph_json":"https://pith.science/api/pith-number/26B75WXZ7ZFIOHAPRDWX2VQIGM/graph.json","events_json":"https://pith.science/api/pith-number/26B75WXZ7ZFIOHAPRDWX2VQIGM/events.json","paper":"https://pith.science/paper/26B75WXZ"},"agent_actions":{"view_html":"https://pith.science/pith/26B75WXZ7ZFIOHAPRDWX2VQIGM","download_json":"https://pith.science/pith/26B75WXZ7ZFIOHAPRDWX2VQIGM.json","view_paper":"https://pith.science/paper/26B75WXZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2207.02433&json=true","fetch_graph":"https://pith.science/api/pith-number/26B75WXZ7ZFIOHAPRDWX2VQIGM/graph.json","fetch_events":"https://pith.science/api/pith-number/26B75WXZ7ZFIOHAPRDWX2VQIGM/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/26B75WXZ7ZFIOHAPRDWX2VQIGM/action/timestamp_anchor","attest_storage":"https://pith.science/pith/26B75WXZ7ZFIOHAPRDWX2VQIGM/action/storage_attestation","attest_author":"https://pith.science/pith/26B75WXZ7ZFIOHAPRDWX2VQIGM/action/author_attestation","sign_citation":"https://pith.science/pith/26B75WXZ7ZFIOHAPRDWX2VQIGM/action/citation_signature","submit_replication":"https://pith.science/pith/26B75WXZ7ZFIOHAPRDWX2VQIGM/action/replication_record"}},"created_at":"2026-07-05T04:38:03.090742+00:00","updated_at":"2026-07-05T04:38:03.090742+00:00"}