{"main_file_link":[{"url":"https://doi.org/10.1007/s10701-018-0201-0"}],"year":"2018","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","intvolume":"        48","volume":48,"page":"1430-1445","citation":{"short":"Z. Haiman, Foundations of Physics 48 (2018) 1430–1445.","mla":"Haiman, Zoltán. “The X-Ray Chirp of a Compact Black Hole Binary.” <i>Foundations of Physics</i>, vol. 48, no. 10, Springer Science and Business Media LLC, 2018, pp. 1430–45, doi:<a href=\"https://doi.org/10.1007/s10701-018-0201-0\">10.1007/s10701-018-0201-0</a>.","chicago":"Haiman, Zoltán. “The X-Ray Chirp of a Compact Black Hole Binary.” <i>Foundations of Physics</i>. Springer Science and Business Media LLC, 2018. <a href=\"https://doi.org/10.1007/s10701-018-0201-0\">https://doi.org/10.1007/s10701-018-0201-0</a>.","ama":"Haiman Z. The X-ray chirp of a compact black hole binary. <i>Foundations of Physics</i>. 2018;48(10):1430-1445. doi:<a href=\"https://doi.org/10.1007/s10701-018-0201-0\">10.1007/s10701-018-0201-0</a>","apa":"Haiman, Z. (2018). The X-ray chirp of a compact black hole binary. <i>Foundations of Physics</i>. Springer Science and Business Media LLC. <a href=\"https://doi.org/10.1007/s10701-018-0201-0\">https://doi.org/10.1007/s10701-018-0201-0</a>","ieee":"Z. Haiman, “The X-ray chirp of a compact black hole binary,” <i>Foundations of Physics</i>, vol. 48, no. 10. Springer Science and Business Media LLC, pp. 1430–1445, 2018.","ista":"Haiman Z. 2018. The X-ray chirp of a compact black hole binary. Foundations of Physics. 48(10), 1430–1445."},"type":"journal_article","month":"07","scopus_import":"1","abstract":[{"text":"The gravitational waves (GWs) from a binary black hole with masses 10^4≲ M≲ 10^7M_⊙ can be detected with the Laser Interferometer Space Antenna (LISA) once their orbital frequency exceeds 10^{-4}-10^{-5} Hz. The binary separation at this stage is a=O(100)Rg (gravitational radius), and the orbital speed is v/c=O(0.1). I argue that at this stage, the binary will be producing bright electromagnetic (EM) radiation via gas bound to the individual BHs. Both BHs will have their own photospheres in X-ray and possibly also in optical bands. Relativistic Doppler modulations and lensing effects will inevitably imprint periodic variability in the EM light-curve, tracking the phase of the orbital motion, and serving as a template for the GW inspiral waveform. Advanced localization of the source by LISA weeks to months prior to merger will enable a measurement of this EM chirp by wide-field X-ray or optical instruments. A comparison of the phases of the GW and EM chirp signals will help break degeneracies between system parameters, and probe a fractional difference difference Δ v in the propagation speed of photons and gravitons as low as Δ v/c ≈ 10^{-17}.","lang":"eng"}],"date_published":"2018-07-31T00:00:00Z","publication":"Foundations of Physics","_id":"17612","date_created":"2024-09-05T13:24:36Z","publication_status":"published","extern":"1","article_processing_charge":"No","publication_identifier":{"issn":["0015-9018","1572-9516"]},"status":"public","article_type":"original","publisher":"Springer Science and Business Media LLC","alternative_title":["A Phase Template for the Gravitational Wave Inspiral"],"title":"The X-ray chirp of a compact black hole binary","issue":"10","date_updated":"2024-09-24T07:28:50Z","oa_version":"None","author":[{"first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","full_name":"Haiman, Zoltán"}],"doi":"10.1007/s10701-018-0201-0","quality_controlled":"1","language":[{"iso":"eng"}],"day":"31"}