{"paper":{"title":"Formation and coalescence of relativistic binary stars: effect of kick velocity","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"K.A. Postnov, M.E. Prokhorov (Sternberg Astronomical Institute, Moscow, Russia), V.M. Lipunov","submitted_at":"1997-02-06T14:13:12Z","abstract_excerpt":"Galactic binary pulsars with different companion types (OB-star, white dwarf (WD), neutron star (NS), black hole (BH), or planet) assuming various phenomenological distributions for kick velocities of newborn NS are studied.\n  The merging rates of relativistic binary stars (NS+NS, NS+BH, BH+BH) dependence on the kick velocity is specially adresed. The BH+BH merging is shown to occur, depending on parameters of BH formation, at a rate of one per 200,000 -- 500,000 years in a Milky Way type galaxy. The NS+NS merging rate $R_{ns}$ is found to be 1 per \\sim 3,000 years for zero recoil, and decreas"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9702060","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"}