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Interacting white dwarf binary star systems, including helium cataclysmicvariable (HeCV) systems, are expected to be strong sources of gravitationalradiation, and should be detectable by proposed space-based laserinterferometer gravitational wave observatories such as LISA. Several HeCV starsystems are presently known and can be studied optically, which will allowelectromagnetic and gravitational wave observations to be correlated.Comparisons of the phases of a gravitational wave signal and the orbital lightcurve from an interacting binary white dwarf star system can be used to boundthe mass of the graviton. Observations of typical HeCV systems by LISA couldpotentially yield an upper bound on the inverse mass of the graviton as strongas $h/m_{g} = \lambda_{g} > 1 \times 10^{15}$ km ($m_{g} < 1 \times 10^{-24}$eV), more than two orders of magnitude better than present solar system derivedbounds.Comment: 21 pages plus 4 figures; ReVTe

Using binary stars to bound the mass of the graviton