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The discovery of the most compact detached white dwarf (WD) binary SDSSJ065133.33+284423.3 has been discussed in terms of probing the tidal effects inwhite dwarfs. This system is also a verification source for the space-basedgravitational wave (GW) detector, evolved Laser Interferometer Space Antenna(eLISA) which will observe short-period compact Galactic binaries with$P_{orb}\lesssim 5$ hrs. We address the prospects of doing tidal studies usingeLISA binaries by showing the fractional uncertainties in the orbital decayrate and the rate of that decay, $\dot{f}, \ddot{f}$ expected from both the GWand EM data for some of the high-$f$ binaries. We find that $\dot{f}$ and$\ddot{f}$ can be measured using GW data only for the most massive WD binariesobserved at high-frequencies. Form timing the eclipses for $\sim 10$ years, wefind that $\dot{f}$ can be known to $\sim 0.1% $ for J0651. We find that fromGW data alone, measuring the effects of tides in binaries is (almost)impossible. We also investigate the improvement in the knowledge of the binaryparameters by combining GW amplitude and inclination with EM data with andwithout $\dot{f}$. In our previous work we found that EM data on distanceconstrained 2-$\sigma$ uncertainty in chirp mass to $15-25%$ whereas adding$\dot{f}$ reduces it to $0.11%$. EM data on $\dot{f}$ also constrains2-$\sigma$ uncertainty in distance to $35%-19%$. EM data on primary massconstrains the secondary mass $m_2$ to factors of 2 to $\sim40%$ whereas adding$\dot{f}$ reduces this to $25%$. And finally using single-line spectroscopicconstrains 2-$\sigma$ uncertainties in both the $m_2, d$ to factors of 2 to$\sim 40%$. Adding EM data on $\dot{f}$ reduces these 2-$\sigma$ uncertaintiesto $\leq 25%$ and $6%-19%$ respectively. Thus we find that EM measurements of$\dot{f}$ and radial velocity will be valuable in constraining binaryparameters.

Measuring tides and binary parameters from gravitational wave data and eclipsing timings of detached white dwarf binaries