{"record":{"author":{"account_ref":null,"orcid":null},"builds_on":[],"content_schema":"pubphys.content.topic/1","content_sha256":"7d9c358412e750b13cfac4f60802b48de8818521a5bdb0e668cb0100653bd957","created":"2026-10-03T07:17:51Z","files":[],"origin":{"assisted_by":[],"kind":"seed"},"parents":[],"salt":"0bf5689c8b49bf806b88d81a7a52b3208e13d89cbf0c17155d196058cc34a73b","schema":"pubphys.record/2","site":"pubphys.com","target":null,"type":"topic"},"content":{"external_id":"cosmo.galaxy-scale-dark-matter","field":"cosmo","n":"1","review_cite":"Bullock J.S., Boylan-Kolchin M., Small-Scale Challenges to the LCDM Paradigm, Annual Review of Astronomy and Astrophysics, 2017","review_link":"https://arxiv.org/abs/1707.04256","review_verified":"true","summary":"Simulations of cold dark matter predict how mass is arranged inside galaxies, and some observations of small galaxies disagree in detail. Galaxies also obey tight empirical rules linking their visible matter to their total gravity, rules that MOND (modified Newtonian dynamics, a change of gravity at very low accelerations) builds in from the start.","title":"Dark matter in galaxies and MOND phenomenology","topic_ref":null,"why":"Galaxy scales are where cold dark matter is most likely to fail and where alternative dark matter physics or modified gravity would leave signatures."},"attested":{"attestation":{"batch":null,"client_id":null,"id_token_sha256":null,"kind":"platform"},"record_hash":"2930612cbb6d87e36edabf652b28a9ef16183bca601f4a29730a1ed3093544bf","schema":"pubphys.attested/1"},"envelope":{"attested_hash":"bba5c50692430085eb509216035e3c8945f9b675677d257a9faf34c871993176","platform_signature":{"key_id":"c6afc19b31429869751f06879c75cd64ea92654423d15b44be775bf1310a60da","sig":"6U-_SzU3gKkWazGyFULkSb57O-sMiFKmocliQ8WnQ0oHLos5dc-O-NW2HuEZQakrDF0LJO73q6tBaV4ibuNYDw"},"schema":"pubphys.envelope/1"},"record_hash":"2930612cbb6d87e36edabf652b28a9ef16183bca601f4a29730a1ed3093544bf","leaf_index":187}