Using binary stars to bound the mass of the graviton

Details Using binary stars to bound the mass of the graviton Using binary stars to bound the mass of the graviton

1999-12-23

arxiv.org/abs/gr-qc/9912102v1

Phys.Rev. D61 (2000) 104008

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

21 pages plus 4 figures; ReVTeX

Scientific paper

10.1103/PhysRevD.61.104008

Interacting white dwarf binary star systems, including helium cataclysmic variable (HeCV) systems, are expected to be strong sources of gravitational radiation, and should be detectable by proposed space-based laser interferometer gravitational wave observatories such as LISA. Several HeCV star systems are presently known and can be studied optically, which will allow electromagnetic and gravitational wave observations to be correlated. Comparisons of the phases of a gravitational wave signal and the orbital light curve from an interacting binary white dwarf star system can be used to bound the mass of the graviton. Observations of typical HeCV systems by LISA could potentially yield an upper bound on the inverse mass of the graviton as strong as $h/m_{g} = \lambda_{g} > 1 \times 10^{15}$ km ($m_{g} < 1 \times 10^{-24}$ eV), more than two orders of magnitude better than present solar system derived bounds.

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