Bounding the graviton mass with binary pulsar observations

Abstract

By comparing the observed orbital decay of the binary pulsars PSRB1913+16 and PSRB1534+12 to that predicted by general relativity due to gravitational-wave emission, we are able to bound the mass of the graviton to be less than $7.6\times 10^{-20}\text{eV}/c^2$ at 90% confidence. This is the first such bound to be derived from dynamic gravitational fields. It is approximately two orders of magnitude weaker than the static-field bound from solar system observations, and will improve with further observations.

9 pages, 1 figure. Presented at Fourth Edoardo Amaldi Conference on Gravitational Waves, Perth, 2001

References in corpus (4)

• A Unified Approach to the Classical Statistical Analysis of Small Signals
• Bounding the mass of the graviton using gravitional-wave observations of inspiralling compact binaries
• Using binary stars to bound the mass of the graviton
• Recent Arecibo Timing of the Relativistic Binary PSR B1534+12

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• Pulsar timing array observations of gravitational wave source timing parallax
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• Effective Field Theory of Broken Spatial Diffeomorphisms
• Graviton Mass from Close White Dwarf Binaries Detectable with LISA
• Bounding the mass of graviton in a dynamic regime with binary pulsars
• Resonant Primordial Gravitational Waves Amplification
• The conservation of energy-momentum and the mass for the graviton