  T Aurigae is an eclipsing old nova which exploded in 1891. At a Gaia EDR3
distance of 815-871 pc, it is a relatively nearby old nova. Through ultraviolet
spectral modeling and using the new precise Gaia distance, we find that the
HST/STIS spectrum of T Aurigae is consistent with an accretion disk with a mass
transfer rate $\dot{M}$ of the order of $10^{-8}M_{\odot}$/yr, for a white
dwarf mass of $M_{\rm wd} \approx 0.7 \pm 0.2 M_{\odot}$, an inclination of $i
\sim 60^{\circ}$, and a Gaia distance of of $840_{-25}^{+31}$~pc. The sharp
absorption lines of metals cannot form in the disk and are likely forming in
material above the disk (e.g. due stream disk overflow), in circumbinary
material, and/or in material associated with the ejected shell from the 1891
nova explosion. The saturated hydrogen Ly$\alpha$ absorption feature is
attributed to a large interstellar medium hydrogen column density of the order
of $10^{21}$cm$^{-2}$ towards T Aur, as corroborated by the value of its
reddening $E(B-V)=0.42 \pm 0.08$.
