{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:3WEDI54Z54QDXPV3TDQM2VZ5KD","short_pith_number":"pith:3WEDI54Z","schema_version":"1.0","canonical_sha256":"dd88347799ef203bbebb98e0cd573d50f0b8058116e30918497456e231b29f8d","source":{"kind":"arxiv","id":"1907.05785","version":1},"attestation_state":"computed","paper":{"title":"Asymmetric Dark Matter Imprint on Low-mass Main-sequence Stars in the Milky Way Nuclear Star Cluster","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Il\\'idio Lopes, Jos\\'e Lopes","submitted_at":"2019-07-12T15:18:15Z","abstract_excerpt":"In this work, we study the impact of asymmetric dark matter (ADM) on low-mass main-sequence stars in the Milky Way's nuclear star cluster, where the dark matter (DM) density is expected to be orders of magnitude above what is found near the Sun (${\\rho }_{\\mathrm{DM}}\\gtrsim {10}^{3}\\ \\mathrm{GeV}\\ {\\mathrm{cm}}^{-3}$). Using a modified stellar evolution code and considering a DM particle ($m_{\\chi} = 4 \\text{ GeV}$) with a spin-dependent interaction cross section close to the limits allowed by direct detection, we found that the interactions of ADM with baryons in the star's core can have two"},"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":"1907.05785","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2019-07-12T15:18:15Z","cross_cats_sorted":[],"title_canon_sha256":"7a44813574d38a6fbe1b163df32eed03eb84b3c23869fac0a4da131546c531e0","abstract_canon_sha256":"a80defcd1c5e9d99d7bd5f2641fd5f0157843cec31080772bcad78ddd79dce07"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:40:44.417458Z","signature_b64":"30z7i/ymKyJAwkwsujo0Gq43E3Pwzy+bdtlUG3J3CfiCxf8ivduZ08orafv9Zy5ZMDAKW1ONaziEP/fzs+SNAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"dd88347799ef203bbebb98e0cd573d50f0b8058116e30918497456e231b29f8d","last_reissued_at":"2026-05-17T23:40:44.416446Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:40:44.416446Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Asymmetric Dark Matter Imprint on Low-mass Main-sequence Stars in the Milky Way Nuclear Star Cluster","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Il\\'idio Lopes, Jos\\'e Lopes","submitted_at":"2019-07-12T15:18:15Z","abstract_excerpt":"In this work, we study the impact of asymmetric dark matter (ADM) on low-mass main-sequence stars in the Milky Way's nuclear star cluster, where the dark matter (DM) density is expected to be orders of magnitude above what is found near the Sun (${\\rho }_{\\mathrm{DM}}\\gtrsim {10}^{3}\\ \\mathrm{GeV}\\ {\\mathrm{cm}}^{-3}$). Using a modified stellar evolution code and considering a DM particle ($m_{\\chi} = 4 \\text{ GeV}$) with a spin-dependent interaction cross section close to the limits allowed by direct detection, we found that the interactions of ADM with baryons in the star's core can have two"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1907.05785","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":"1907.05785","created_at":"2026-05-17T23:40:44.416615+00:00"},{"alias_kind":"arxiv_version","alias_value":"1907.05785v1","created_at":"2026-05-17T23:40:44.416615+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1907.05785","created_at":"2026-05-17T23:40:44.416615+00:00"},{"alias_kind":"pith_short_12","alias_value":"3WEDI54Z54QD","created_at":"2026-05-18T12:33:10.108867+00:00"},{"alias_kind":"pith_short_16","alias_value":"3WEDI54Z54QDXPV3","created_at":"2026-05-18T12:33:10.108867+00:00"},{"alias_kind":"pith_short_8","alias_value":"3WEDI54Z","created_at":"2026-05-18T12:33:10.108867+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2509.03388","citing_title":"Probing Heavy Dark Matter in Red Giants","ref_index":28,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/3WEDI54Z54QDXPV3TDQM2VZ5KD","json":"https://pith.science/pith/3WEDI54Z54QDXPV3TDQM2VZ5KD.json","graph_json":"https://pith.science/api/pith-number/3WEDI54Z54QDXPV3TDQM2VZ5KD/graph.json","events_json":"https://pith.science/api/pith-number/3WEDI54Z54QDXPV3TDQM2VZ5KD/events.json","paper":"https://pith.science/paper/3WEDI54Z"},"agent_actions":{"view_html":"https://pith.science/pith/3WEDI54Z54QDXPV3TDQM2VZ5KD","download_json":"https://pith.science/pith/3WEDI54Z54QDXPV3TDQM2VZ5KD.json","view_paper":"https://pith.science/paper/3WEDI54Z","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1907.05785&json=true","fetch_graph":"https://pith.science/api/pith-number/3WEDI54Z54QDXPV3TDQM2VZ5KD/graph.json","fetch_events":"https://pith.science/api/pith-number/3WEDI54Z54QDXPV3TDQM2VZ5KD/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/3WEDI54Z54QDXPV3TDQM2VZ5KD/action/timestamp_anchor","attest_storage":"https://pith.science/pith/3WEDI54Z54QDXPV3TDQM2VZ5KD/action/storage_attestation","attest_author":"https://pith.science/pith/3WEDI54Z54QDXPV3TDQM2VZ5KD/action/author_attestation","sign_citation":"https://pith.science/pith/3WEDI54Z54QDXPV3TDQM2VZ5KD/action/citation_signature","submit_replication":"https://pith.science/pith/3WEDI54Z54QDXPV3TDQM2VZ5KD/action/replication_record"}},"created_at":"2026-05-17T23:40:44.416615+00:00","updated_at":"2026-05-17T23:40:44.416615+00:00"}