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Galactic interacting double white dwarfs (DWD) are guaranteed gravitationalwave (GW) sources for the GW detector LISA, with more than 10^4 binariesexpected to be detected over the mission's lifetime. Part of this population isexpected to be eccentric, and here we investigate the potential forconstraining the white dwarf (WD) properties through apsidal precession inthese binaries. We analyze the tidal, rotational, and general relativisticcontributions to apsidal precession by using detailed He WD models, where theevolution of the star's interior is followed throughout the cooling phase. Inagreement with previous studies of zero-temperature WDs, we find that apsidalprecession in eccentric DWDs can lead to a detectable shift in the emitted GWsignal when binaries with cool (old) components are considered. This shiftincreases significantly for hot (young) WDs. We find that apsidal motion in hot(cool) DWDs is dominated by tides at orbital frequencies above ~10^{-4}Hz(10^{- 3}$Hz). The analysis of apsidal precession in these sources whileignoring the tidal component would lead to an extreme bias in the massdetermination, and could lead us to misidentify WDs as neutron stars or blackholes. We use the detailed WD models to show that for older, cold WDs, there isa unique relationship that ties the radius and apsidal precession constant tothe WD masses, therefore allowing tides to be used as a tool to constrain thesource masses.

Tidally-Induced Apsidal Precession in Double White Dwarfs: a new mass measurement tool with LISA