  The largest asteroids in the Koronis family (sizes $\geq 25$ km) have very
peculiar rotation state properties, with the retrograde- and prograde-rotating
objects being distinctly different. A recent e-analysis of observations
suggests that one of the asteroids formerly thought to be retrograde-rotating,
208~Lacrimosa, in reality exhibits prograde rotation, yet other properties of
this object are discrepant with other members this group. We seek to understand
whether the new spin solution of Lacrimosa invalidates the previously proposed
model of the Koronis large members or simply reveals more possibilities for the
long-term evolutionary paths, including some that have not yet been explored.
We confirm and substantiate the previously suggested prograde rotation of
Lacrimosa. Its spin vector has an ecliptic longitude and latitude of
$(\lambda,\beta)=(15^\circ \pm 2^\circ, 67^\circ\pm 2^\circ)$ and a sidereal
rotation period $P=14.085734\pm 0.000007$ hr. The thermal and occultation data
allow us to calibrate a volume equivalent size of $D=44\pm 2$ km of Lacrimosa.
The observations also constrain the shape model relatively well. Assuming
uniform density, the dynamical ellipticity is $\Delta=0.35\pm 0.05$. Unlike
other large prograde-rotating Koronis members, Lacrimosa spin is not captured
in the Slivan state. We propose that Lacrimosa differed from this group in that
it had initially slightly larger obliquity and longer rotation period. With
those parameters, it jumped over the Slivan state instead of being captured and
slowly evolved into the present spin configuration. In the future, it is likely
to be captured in the Slivan state corresponding to the proper (instead of
forced) mode of the orbital plane precession in the inertial space.
