  We derive astrophysical parameters of the open cluster NGC 1513 by means of
colour indices built with new $CCD\,UBV(RI)_{KC}$ photometry. Based on
early-type members, the mean foreground reddening and total to selective
extinction ratio are E(B-V)=0.79$\pm$0.09 mag and $R_{V}$=2.85$\pm$0.05.
Through the differential grid method, we derive the metal abundance
[Fe/H]=-0.06 dex (Z=+0.013), which is consistent with the value [Fe/H]=-0.088
of the bright giant member-LAMOST-695710060. The Z=+0.013 isochrone fit to the
V x (B-V) colour-magnitude diagram leads to a turn-off age of 224$\pm$27 Myr
(thus an intermediate-age cluster), and a distance modulus of ($V_{0}$ -
$M_{\rm V}$)=10.90$\pm$0.15 mag, thus implying a distance from the Sun
d=1514$\pm$105 pc. Within the uncertainties, our photometric distance is
consistent with the value d=1435$\pm$14 pc from the Gaia DR3 parallax. We find
signs of small mass segregation through a minimum spanning tree analysis for
the 190 most massive stars, together with the rather steep mass function
($\chi$=+2.39) slope. The high core to half-light radius ratio
$R_{core}$/$R_{h}$=0.82, together with the compact half-light to tidal radius
ratio $R_{h}$/$R_{t}$=0.22, suggest that it is probably related to
cluster-formation effects, due to little dynamical evolution, instead of
driving its dynamical evolution by internal relaxation. Indeed, NGC 1513 is
located in the second quadrant ($\ell$=152.59$^{\circ}$ and Galactocentric
distance $R_{GC}$=9.57 kpc), which tends to minimize tidal effects by external
processes and tidal disruption. Therefore, internal mass segregation effects in
NGC 1513 seem to be more efficient than cluster evaporation processes. We find
that NGC 1513 migrated about 0.50 kpc from its birth place.
