We present new photometry and spectroscopy of the 94m eclipsing binary LSQ1725-64 that provide insight into the fundamental parameters and evolutionary state of this system .
We confirm that LSQ1725-64 is a magnetic cataclysmic variable whose white dwarf has a surface-averaged magnetic field strength of 12.5 \pm 0.5 MG measured from Zeeman splitting .
The spectral type and colour of the secondary , as well as the eclipse length , are consistent with other secondaries that have not yet evolved through the period minimum expected for cataclysmic variables .
We observe two different states of mass transfer and measure the transition between the two to occur over about 45 orbital cycles .
In the low state , we observe photometric variations that we hypothesize to arise predominantly from two previously heated magnetic poles of the white dwarf .
Our precise eclipse measurements allow us to determine binary parameters of LSQ1725-64 and we find it contains a high mass ( 0.97 \pm 0.03 M _ { \odot } ) white dwarf if we assume a typical mass-radius relationship for a CO core white dwarf .
We also measure an eclipse of the accretion stream after the white dwarf eclipse , and use it to estimate an upper limit of the mass transfer rate .
This derived limit is consistent with that expected from angular momentum loss via gravitational radiation alone .