{"record":{"author":{"account_ref":null,"orcid":null},"builds_on":[],"content_schema":"pubphys.content.revision/1","content_sha256":"b461ceaaa225092e1389444a7f7c0861b8e40c55affd264413f8a256955f9ffc","created":"2026-10-03T07:17:55Z","files":[],"origin":{"assisted_by":[],"kind":"seed"},"parents":["5475cf5dc5b1a72283d26dc95dc6e00d7ea4e00096a7c6492e409a1816eeb011"],"salt":"0b83a78e9b151dfedf833cb248fdac6b85eb4fb405f7386819dc5a72bc5af5ed","schema":"pubphys.record/2","site":"pubphys.com","target":null,"type":"revision"},"content":{"answer_type":"mechanism","assisted_by":[],"external_id":"astro.neutron-star-interiors.r-mode-instability","kind":"phenomenon","literature_status":"open","n":"1","parents":[],"plain":"Theory says certain sloshing oscillations called r-modes should grow on their own in fast-spinning neutron stars, radiate gravitational waves and slow the stars down. Yet many observed stars spin fast in the region where this should happen.","posed_since":"","precise":"With standard shear and bulk viscosity, low-mass X-ray binaries spinning at $300\\ \\text{to}\\ 700\\ \\mathrm{Hz}$ with inferred core temperatures of about $1e8\\ \\mathrm{K}$ lie inside the r-mode instability window. Determine the extra damping (viscous crust-core boundary layer, hyperon or quark bulk viscosity, superfluid mutual friction, resonances) or the low saturation amplitude that reconciles theory with the observed spin and temperature distribution.","problem_ref":null,"references":"","settled_by":"A calculation of r-mode damping and nonlinear saturation in realistic stellar models that places the observed systems outside the window or predicts their spin-temperature distribution.","status_note":"","title":"Why do fast-spinning accreting neutron stars evade the r-mode instability?","topic_ref":"afd1feb0d7ec84994296c83f9c2ecba96e22fc9ddf5d5fa7c0562e1f6f4eb1d4"},"attested":{"attestation":{"batch":null,"client_id":null,"id_token_sha256":null,"kind":"platform"},"record_hash":"d826b7bb33a13e474e94155f77b7835fdfbc48296f3beafd9225fefb8e1acae8","schema":"pubphys.attested/1"},"envelope":{"attested_hash":"aecb450b4eff60c2d274564c28700f010b55c6b28df746adb96a34090f7b2f00","platform_signature":{"key_id":"c6afc19b31429869751f06879c75cd64ea92654423d15b44be775bf1310a60da","sig":"Wienz9IEH6Gnwq4wxzlHY7VxE3vSihhEqNbaP72FvA2-vusuRP87f9ENr9qw08yZTc6if7xzIJZUpPltsOQcDQ"},"schema":"pubphys.envelope/1"},"record_hash":"d826b7bb33a13e474e94155f77b7835fdfbc48296f3beafd9225fefb8e1acae8","leaf_index":574}