  We comment on a recent study reporting evidence for the general relativistic
Lense-Thirring secular precession of the inclination $I$ of the orbital plane
to the plane of the sky of the tight binary system PSR J1141-6545 made of a
white dwarf and an emitting radiopulsar of comparable masses. The quadrupole
mass moment $Q_2^\mathrm{c}$ and the angular momentum ${\boldsymbol
S}^\mathrm{c}$ of the white dwarf cause the detectable effects on $I$ with
respect to the present-day accuracy in the pulsar's timing. The
history-dependent and model-dependent assumptions to be made on
$Q_2^\mathrm{c}$ and ${\boldsymbol S}^\mathrm{c}$, required even just to
calculate the analytical expressions for the resulting post-Keplerian
precessions, may be deemed as too wide in order to claim a successful test of
the Einsteinian gravitomagnetic effect. Moreover, depending on how
$Q_2^\mathrm{c}$ is calculated, the competing quadrupole-induced rate of
change, which is a major source of systematic uncertainty, may be up to
$\lesssim 30-50\%$ of the Lense-Thirring effect for most of the allowed values
in the 3D parameter space spanned by the white dwarf's spin period
$P_\mathrm{s}$, and the polar angles $i_\mathrm{c},\,\zeta_\mathrm{c}$ of its
spin axis. The possible use of the longitude of periastron $\dot\varpi$ is
investigated as well. It turns out that a measurement of its secular
precession, caused, among other things, also by
$Q_2^\mathrm{c},\,{\boldsymbol{S}}^\mathrm{c}$, could help in further
restricting the permitted regions in the white dwarf's parameter space.
