{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:C2BKTXVWVGCCVWUFH3MNKCKTXY","short_pith_number":"pith:C2BKTXVW","schema_version":"1.0","canonical_sha256":"1682a9deb6a9842ada853ed8d50953be2451ac8a6823368a3df787f2b27789bc","source":{"kind":"arxiv","id":"2005.05946","version":2},"attestation_state":"computed","paper":{"title":"Comment on \"Multiscatter stellar capture of dark matter\"","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","astro-ph.SR","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Cosmin Ilie, Jacob Pilawa, Saiyang Zhang","submitted_at":"2020-05-12T17:47:01Z","abstract_excerpt":"Bramante, Delgado, and Martin [Phys. Rev. D96, 063002(2017)., hereafter BDM17] extended the analytical formalism of dark matter (DM) capture in a very important way, which allows, in principle, the use of compact astrophysical objects, such as neutron stars (NS), as dark matter detectors. In this comment, we point out the existence of a region in the dark matter neutron scattering cross section $(\\sigma_{nX})$ vs. dark matter mass $(m_{X})$ where the constraining power of this method is lost. This corresponds to a maximal temperature ($T_{crit}$) the NS has to have, in order to serve as a dark"},"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":"2005.05946","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2020-05-12T17:47:01Z","cross_cats_sorted":["astro-ph.HE","astro-ph.SR","hep-ph"],"title_canon_sha256":"98cac77a3f30e8d2fcfb5b47aa973f9e03781048e21297a9734385ba97239228","abstract_canon_sha256":"e395f00c039b825fc35097ee72dbeee53d8350543b6a5fbee491ebf04888388a"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T01:32:04.603262Z","signature_b64":"dStGCZuO4ZT5Du3JwYZSj4ofhwBCnC/cMCGQFoXn8P02RwJ84WbBr7814+n20G9HnGkd9H8C4ZMyA4US9jPpBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"1682a9deb6a9842ada853ed8d50953be2451ac8a6823368a3df787f2b27789bc","last_reissued_at":"2026-07-05T01:32:04.602874Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T01:32:04.602874Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Comment on \"Multiscatter stellar capture of dark matter\"","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","astro-ph.SR","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Cosmin Ilie, Jacob Pilawa, Saiyang Zhang","submitted_at":"2020-05-12T17:47:01Z","abstract_excerpt":"Bramante, Delgado, and Martin [Phys. Rev. D96, 063002(2017)., hereafter BDM17] extended the analytical formalism of dark matter (DM) capture in a very important way, which allows, in principle, the use of compact astrophysical objects, such as neutron stars (NS), as dark matter detectors. In this comment, we point out the existence of a region in the dark matter neutron scattering cross section $(\\sigma_{nX})$ vs. dark matter mass $(m_{X})$ where the constraining power of this method is lost. This corresponds to a maximal temperature ($T_{crit}$) the NS has to have, in order to serve as a dark"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2005.05946","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/2005.05946/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":"2005.05946","created_at":"2026-07-05T01:32:04.602931+00:00"},{"alias_kind":"arxiv_version","alias_value":"2005.05946v2","created_at":"2026-07-05T01:32:04.602931+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2005.05946","created_at":"2026-07-05T01:32:04.602931+00:00"},{"alias_kind":"pith_short_12","alias_value":"C2BKTXVWVGCC","created_at":"2026-07-05T01:32:04.602931+00:00"},{"alias_kind":"pith_short_16","alias_value":"C2BKTXVWVGCCVWUF","created_at":"2026-07-05T01:32:04.602931+00:00"},{"alias_kind":"pith_short_8","alias_value":"C2BKTXVW","created_at":"2026-07-05T01:32:04.602931+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.21652","citing_title":"Constraining dark matter self-interaction from kinetic heating in neutron stars","ref_index":27,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/C2BKTXVWVGCCVWUFH3MNKCKTXY","json":"https://pith.science/pith/C2BKTXVWVGCCVWUFH3MNKCKTXY.json","graph_json":"https://pith.science/api/pith-number/C2BKTXVWVGCCVWUFH3MNKCKTXY/graph.json","events_json":"https://pith.science/api/pith-number/C2BKTXVWVGCCVWUFH3MNKCKTXY/events.json","paper":"https://pith.science/paper/C2BKTXVW"},"agent_actions":{"view_html":"https://pith.science/pith/C2BKTXVWVGCCVWUFH3MNKCKTXY","download_json":"https://pith.science/pith/C2BKTXVWVGCCVWUFH3MNKCKTXY.json","view_paper":"https://pith.science/paper/C2BKTXVW","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2005.05946&json=true","fetch_graph":"https://pith.science/api/pith-number/C2BKTXVWVGCCVWUFH3MNKCKTXY/graph.json","fetch_events":"https://pith.science/api/pith-number/C2BKTXVWVGCCVWUFH3MNKCKTXY/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/C2BKTXVWVGCCVWUFH3MNKCKTXY/action/timestamp_anchor","attest_storage":"https://pith.science/pith/C2BKTXVWVGCCVWUFH3MNKCKTXY/action/storage_attestation","attest_author":"https://pith.science/pith/C2BKTXVWVGCCVWUFH3MNKCKTXY/action/author_attestation","sign_citation":"https://pith.science/pith/C2BKTXVWVGCCVWUFH3MNKCKTXY/action/citation_signature","submit_replication":"https://pith.science/pith/C2BKTXVWVGCCVWUFH3MNKCKTXY/action/replication_record"}},"created_at":"2026-07-05T01:32:04.602931+00:00","updated_at":"2026-07-05T01:32:04.602931+00:00"}