{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:R6M535NC4SFCAY3H7YCQEIFEB4","short_pith_number":"pith:R6M535NC","schema_version":"1.0","canonical_sha256":"8f99ddf5a2e48a206367fe050220a40f12b9e9b8163f80373aac5f0cf48d7f19","source":{"kind":"arxiv","id":"2204.05560","version":2},"attestation_state":"computed","paper":{"title":"Dark matter admixed neutron star properties in the light of X-ray pulse profile observations","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.SR","hep-ph","nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"Ang Li, Feng Huang, Yaofeng Zhu, Zhiqiang Miao","submitted_at":"2022-04-12T06:46:17Z","abstract_excerpt":"The distribution of the dark matter (DM) in DM-admixed-neutron stars (DANSs) is supposed to be either a dense dark core or an extended dark halo, which is subject to the DM fraction of DANS ($f_{\\chi}$) and the DM properties, such as the mass ($m_{\\chi}$) and the strength of the self-interaction ($y$). In this paper, we perform an in-depth analysis of the formation criterion for dark core/dark halo and point out that the relative distribution of these two components is essentially determined by the ratio of the central enthalpy of the DM component to that of the baryonic matter component insid"},"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":"2204.05560","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2022-04-12T06:46:17Z","cross_cats_sorted":["astro-ph.CO","astro-ph.SR","hep-ph","nucl-th"],"title_canon_sha256":"312d1c6354a39f07a65a06a0baa90b756dbd090601f4e9c8d0b3eaa4fe33944a","abstract_canon_sha256":"57775fcbe2caa8c8cf06a82d2b722f272b3022cd58849e753ad58d22c514d9a2"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:54:55.838993Z","signature_b64":"tMEeTWuPbNJnS6vaitYAULFIFFGOJ79H8nD2VIqCSPbxqhW30qvfx3L1wNDGCx+SnU53LW1scBBsssSb8HNMDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8f99ddf5a2e48a206367fe050220a40f12b9e9b8163f80373aac5f0cf48d7f19","last_reissued_at":"2026-07-05T04:54:55.838573Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:54:55.838573Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Dark matter admixed neutron star properties in the light of X-ray pulse profile observations","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.SR","hep-ph","nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"Ang Li, Feng Huang, Yaofeng Zhu, Zhiqiang Miao","submitted_at":"2022-04-12T06:46:17Z","abstract_excerpt":"The distribution of the dark matter (DM) in DM-admixed-neutron stars (DANSs) is supposed to be either a dense dark core or an extended dark halo, which is subject to the DM fraction of DANS ($f_{\\chi}$) and the DM properties, such as the mass ($m_{\\chi}$) and the strength of the self-interaction ($y$). In this paper, we perform an in-depth analysis of the formation criterion for dark core/dark halo and point out that the relative distribution of these two components is essentially determined by the ratio of the central enthalpy of the DM component to that of the baryonic matter component insid"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2204.05560","kind":"arxiv","version":2},"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/2204.05560/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":"2204.05560","created_at":"2026-07-05T04:54:55.838631+00:00"},{"alias_kind":"arxiv_version","alias_value":"2204.05560v2","created_at":"2026-07-05T04:54:55.838631+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2204.05560","created_at":"2026-07-05T04:54:55.838631+00:00"},{"alias_kind":"pith_short_12","alias_value":"R6M535NC4SFC","created_at":"2026-07-05T04:54:55.838631+00:00"},{"alias_kind":"pith_short_16","alias_value":"R6M535NC4SFCAY3H","created_at":"2026-07-05T04:54:55.838631+00:00"},{"alias_kind":"pith_short_8","alias_value":"R6M535NC","created_at":"2026-07-05T04:54:55.838631+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"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":49,"is_internal_anchor":false},{"citing_arxiv_id":"2503.19691","citing_title":"Strongly Interacting Dark Matter admixed Neutron Stars","ref_index":94,"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":25,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/R6M535NC4SFCAY3H7YCQEIFEB4","json":"https://pith.science/pith/R6M535NC4SFCAY3H7YCQEIFEB4.json","graph_json":"https://pith.science/api/pith-number/R6M535NC4SFCAY3H7YCQEIFEB4/graph.json","events_json":"https://pith.science/api/pith-number/R6M535NC4SFCAY3H7YCQEIFEB4/events.json","paper":"https://pith.science/paper/R6M535NC"},"agent_actions":{"view_html":"https://pith.science/pith/R6M535NC4SFCAY3H7YCQEIFEB4","download_json":"https://pith.science/pith/R6M535NC4SFCAY3H7YCQEIFEB4.json","view_paper":"https://pith.science/paper/R6M535NC","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2204.05560&json=true","fetch_graph":"https://pith.science/api/pith-number/R6M535NC4SFCAY3H7YCQEIFEB4/graph.json","fetch_events":"https://pith.science/api/pith-number/R6M535NC4SFCAY3H7YCQEIFEB4/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/R6M535NC4SFCAY3H7YCQEIFEB4/action/timestamp_anchor","attest_storage":"https://pith.science/pith/R6M535NC4SFCAY3H7YCQEIFEB4/action/storage_attestation","attest_author":"https://pith.science/pith/R6M535NC4SFCAY3H7YCQEIFEB4/action/author_attestation","sign_citation":"https://pith.science/pith/R6M535NC4SFCAY3H7YCQEIFEB4/action/citation_signature","submit_replication":"https://pith.science/pith/R6M535NC4SFCAY3H7YCQEIFEB4/action/replication_record"}},"created_at":"2026-07-05T04:54:55.838631+00:00","updated_at":"2026-07-05T04:54:55.838631+00:00"}