Rømer time-delay determination of the gravitational-wave propagation speed

2013/04/01 by L. S. Finn, Lee Samuel Finn, Joseph D. Romano · 9 citations
Earth and Planetary Sciences · Physics and Astronomy · #Advanced Frequency and Time Standards #Astronomy #Detector #Geophysics and Gravity Measurements #Gravitational wave #Gravitational-wave observatory #Jupiter (rocket family) #LIGO #Neutron star #Optics #Physics #Pulsars and Gravitational Waves Research #Space exploration #astro-ph.IM #gr-qc

paper · pdf · doi:10.1103/physrevd.88.022001

published in Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields 88(2) (American Physical Society) · 12 pages, 1 figure, submitted to PRD

arxiv created 2013/04/01 · openalex publication_date 2013/07/09 · arxiv updated 2015/06/15 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05

Abstract

In 1676 Olaus R\omer presented the first observational evidence for a finite light velocity c_em. He formed his estimate by attributing the periodically varying discrepancy between the observed and expected occultation times of the Galilean satellite Io by its planetary host Jupiter to the time it takes light to cross Earth's orbital diameter. Given a stable celestial clock that can be observed in gravitational waves the same principle can be used to measure the propagation speed c_gw of gravitational radiation. Space-based ``LISA''-like detectors will, and terrestrial LIGO-like detectors may, observe such clocks and thus be capable of directly measuring the propagation velocity of gravitational waves. In the case of space-based detectors the clocks will be galactic close white-dwarf binary systems; in the case of terrestrial detectors, the most likely candidate clock is the periodic gravitational radiation from a rapidly rotating nonaxisymmetric neutron star. Here we evaluate the accuracy that may be expected of such a R\omer-type measurement of c_gw by foreseeable future space-based and terrestrial detectors. For space-based, LISA-like detectors, periodic sources are plentiful: by the end of the first year of scientific operations a LISA-like detector will have measured c_gw to better than a part in a thousand. Periodic sources may not be accessible in terrestrial detectors available to us in the foreseeable future; however, if such a source is detected then with a year of observations we could measure c_gw to better than a part in a million.

Citations

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