{"paper":{"title":"Frequency-domain gravitational waveform models for inspiraling binary neutron stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Keisuke Taniguchi, Kenta Kiuchi, Koutarou Kyutoku, Kyohei Kawaguchi, Masaru Shibata, Yuichiro Sekiguchi","submitted_at":"2018-02-19T05:01:50Z","abstract_excerpt":"We develop a model for frequency-domain gravitational waveforms from inspiraling binary neutron stars. Our waveform model is calibrated by comparison with hybrid waveforms constructed from our latest high-precision numerical-relativity waveforms and the SEOBNRv2T waveforms in the frequency range of $10$--$1000\\,{\\rm Hz}$. We show that the phase difference between our waveform model and the hybrid waveforms is always smaller than $0.1\\, {\\rm rad}$ for the binary tidal deformability, ${\\tilde \\Lambda}$, in the range $300\\lesssim{\\tilde \\Lambda}\\lesssim1900$ and for the mass ratio between 0.73 an"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1802.06518","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"}