  We present a census of photometrically detected rotation periods for white
dwarf stars. We analyzed the light curves of 9285 white dwarf stars observed by
the Transiting Exoplanet Survey Satellite (TESS) up to sector 69. Using Fourier
transform analyses and the TESS localize software, we detected variability
periods for 318 white dwarf stars. The 115 high probability likely single white
dwarfs in our sample have a median rotational period of 3.9 hours and a median
absolute deviation of 3.5 h. Our distribution is significantly different from
the distribution of the rotational period from asteroseismology, which exhibits
a longer median period of 24.3 hours and a median absolute deviation of 12.0 h.
In addition, we reported non-pulsating periods for three known pulsating white
dwarfs with rotational period previously determined by asteroseismology: NGC
1501, TIC 7675859, and G226-29. We also calculated evolutionary models that
include six angular momentum transfer mechanisms from the literature throughout
evolution in an attempt to reproduce our findings. Our models indicate that the
temperature-period relation of most observational data is best fitted by models
with low metallicity, probably indicating problems with the computations of
angular-momentum loss during the high-mass-loss phase. Our models also generate
internal magnetic fields through the Tayler-Spruit dynamo.
