{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:ENMOUCSP6UXDFT7ZQA5MMTNSYR","short_pith_number":"pith:ENMOUCSP","schema_version":"1.0","canonical_sha256":"2358ea0a4ff52e32cff9803ac64db2c44cab8fc7e3aa4fa39123bd3a1cf0b578","source":{"kind":"arxiv","id":"1103.5472","version":4},"attestation_state":"computed","paper":{"title":"Constraints on Scalar Asymmetric Dark Matter from Black Hole Formation in Neutron Stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"hep-ph","authors_text":"Hai-Bo Yu, Kathryn M. Zurek, Samuel D. McDermott","submitted_at":"2011-03-28T20:11:07Z","abstract_excerpt":"We consider possibly observable effects of asymmetric dark matter (ADM) in neutron stars. Since dark matter does not self-annihilate in the ADM scenario, dark matter accumulates in neutron stars, eventually reaching the Chandrasekhar limit and forming a black hole. We focus on the case of scalar ADM, where the constraints from Bose-Einstein condensation and subsequent black hole formation are most severe due to the absence of Fermi degeneracy pressure. We also note that in some portions of this constrained parameter space, non-trivial effects from Hawking radiation can modify our limits. We fi"},"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":"1103.5472","kind":"arxiv","version":4},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"hep-ph","submitted_at":"2011-03-28T20:11:07Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"11d2e0c59030b681d5b3ee8994d25ef99b0cac97837c923c80daad22eb832e19","abstract_canon_sha256":"fef1baa7de5ca92a03206558a37d60a9148e3266b949cdc0932fba806a7c9daf"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:03:54.544434Z","signature_b64":"R5t1mPnJMeWGLnVPtRd4HYpOMNYovlGKrQ94JtGr+pSzVAT9FP7EZtP1DRd5eAH4i1Q+BACU2OMKKNuEfr3RDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2358ea0a4ff52e32cff9803ac64db2c44cab8fc7e3aa4fa39123bd3a1cf0b578","last_reissued_at":"2026-05-18T04:03:54.543964Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:03:54.543964Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Constraints on Scalar Asymmetric Dark Matter from Black Hole Formation in Neutron Stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"hep-ph","authors_text":"Hai-Bo Yu, Kathryn M. Zurek, Samuel D. McDermott","submitted_at":"2011-03-28T20:11:07Z","abstract_excerpt":"We consider possibly observable effects of asymmetric dark matter (ADM) in neutron stars. Since dark matter does not self-annihilate in the ADM scenario, dark matter accumulates in neutron stars, eventually reaching the Chandrasekhar limit and forming a black hole. We focus on the case of scalar ADM, where the constraints from Bose-Einstein condensation and subsequent black hole formation are most severe due to the absence of Fermi degeneracy pressure. We also note that in some portions of this constrained parameter space, non-trivial effects from Hawking radiation can modify our limits. We fi"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1103.5472","kind":"arxiv","version":4},"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":"1103.5472","created_at":"2026-05-18T04:03:54.544042+00:00"},{"alias_kind":"arxiv_version","alias_value":"1103.5472v4","created_at":"2026-05-18T04:03:54.544042+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1103.5472","created_at":"2026-05-18T04:03:54.544042+00:00"},{"alias_kind":"pith_short_12","alias_value":"ENMOUCSP6UXD","created_at":"2026-05-18T12:26:28.662955+00:00"},{"alias_kind":"pith_short_16","alias_value":"ENMOUCSP6UXDFT7Z","created_at":"2026-05-18T12:26:28.662955+00:00"},{"alias_kind":"pith_short_8","alias_value":"ENMOUCSP","created_at":"2026-05-18T12:26:28.662955+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2507.15951","citing_title":"Distinguishing Neutron Star vs. Low-Mass Black Hole Binaries with Late Inspiral & Postmerger Gravitational Waves $-$ Sensitivity to Transmuted Black Holes and Non-Annihilating Dark Matter","ref_index":22,"is_internal_anchor":true},{"citing_arxiv_id":"2509.06892","citing_title":"Asymmetric Cannibal Dark Matter: Constraints from Neutron Star","ref_index":9,"is_internal_anchor":true},{"citing_arxiv_id":"2604.21652","citing_title":"Constraining dark matter self-interaction from kinetic heating in neutron stars","ref_index":89,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ENMOUCSP6UXDFT7ZQA5MMTNSYR","json":"https://pith.science/pith/ENMOUCSP6UXDFT7ZQA5MMTNSYR.json","graph_json":"https://pith.science/api/pith-number/ENMOUCSP6UXDFT7ZQA5MMTNSYR/graph.json","events_json":"https://pith.science/api/pith-number/ENMOUCSP6UXDFT7ZQA5MMTNSYR/events.json","paper":"https://pith.science/paper/ENMOUCSP"},"agent_actions":{"view_html":"https://pith.science/pith/ENMOUCSP6UXDFT7ZQA5MMTNSYR","download_json":"https://pith.science/pith/ENMOUCSP6UXDFT7ZQA5MMTNSYR.json","view_paper":"https://pith.science/paper/ENMOUCSP","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1103.5472&json=true","fetch_graph":"https://pith.science/api/pith-number/ENMOUCSP6UXDFT7ZQA5MMTNSYR/graph.json","fetch_events":"https://pith.science/api/pith-number/ENMOUCSP6UXDFT7ZQA5MMTNSYR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ENMOUCSP6UXDFT7ZQA5MMTNSYR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ENMOUCSP6UXDFT7ZQA5MMTNSYR/action/storage_attestation","attest_author":"https://pith.science/pith/ENMOUCSP6UXDFT7ZQA5MMTNSYR/action/author_attestation","sign_citation":"https://pith.science/pith/ENMOUCSP6UXDFT7ZQA5MMTNSYR/action/citation_signature","submit_replication":"https://pith.science/pith/ENMOUCSP6UXDFT7ZQA5MMTNSYR/action/replication_record"}},"created_at":"2026-05-18T04:03:54.544042+00:00","updated_at":"2026-05-18T04:03:54.544042+00:00"}