  We have observed the lightcurves of 13 V-type asteroids ((1933) Tinchen,
(2011) Veteraniya, (2508) Alupka, (3657) Ermolova, (3900) Knezevic, (4005)
Dyagilev, (4383) Suruga, (4434) Nikulin, (4796) Lewis, (6331) 1992
$\mathrm{FZ_{1}}$, (8645) 1998 TN, (10285) Renemichelsen, and (10320) Reiland).
Using these observations we determined the rotational rates of the asteroids,
with the exception of Nikulin and Renemichelsen. The distribution of rotational
rates of 59 V-type asteroids in the inner main belt, including 29 members of
the Vesta family that are regarded as ejecta from the asteroid (4) Vesta, is
inconsistent with the best-fit Maxwellian distribution. This inconsistency may
be due to the effect of thermal radiation
Yarkovsky--O'Keefe--Radzievskii--Paddack (YORP) torques, and implies that the
collision event that formed V-type asteroids is sub-billion to several billion
years in age.
