Maria family is regarded as an old-type ( \sim 3 \pm 1 Gyr ) asteroid family which has experienced substantial collisional and dynamical evolution in the Main-belt .
It is located nearby the 3:1 Jupter mean motion resonance area that supplies Near-Earth asteroids ( NEAs ) to the inner Solar System .
We carried out observations of Maria family asteroids during 134 nights from 2008 July to 2013 May , and derived synodic rotational periods for 51 objects , including newly obtained periods of 34 asteroids .
We found that there is a significant excess of fast and slow rotators in observed rotation rate distribution .
The two-sample Kolmogorov-Smirnov test confirms that the spin rate distribution is not consistent with a Maxwellian at a 92 % confidence level .
From correlations among rotational periods , amplitudes of lightcurves , and sizes , we conclude that the rotational properties of Maria family asteroids have been changed considerably by non-gravitational forces such as the YORP effect .
Using a lightcurve inversion method ( 28 ; 29 ) , we successfully determined the pole orientations for 13 Maria members , and found an excess of prograde versus retrograde spins with a ratio ( N _ { p } / N _ { r } ) of 3 .
This implies that the retrograde rotators could have been ejected by the 3:1 resonance into the inner Solar System since the formation of Maria family .
We estimate that approximately 37 to 75 Maria family asteroids larger than 1 km have entered the near-Earth space every 100 Myr .