  A combination of two unsupervised machine learning algorithms, DBSCAN and GMM
are used to find members with a high probability of twelve open clusters, M38,
NGC2099, Coma Ber, NGC752, M67, NGC2243, Alessi01, Bochum04, M34, M35, M41, and
M48, based on Gaia DR3. These clusters have different ages, distances, and
numbers of members which makes a suitable cover of these parameters situation
to analyze this method. We have identified 752, 1725, 116, 269, 1422, 936, 43,
38, 743, 1114, 783, and 452, probable and possible members with a higher
probability than 0.8 for M38, NGC2099, Coma Ber, NGC752, M67, NGC2243,
Alessi01, Bochum04, M34, M35, M41, and M48, respectively. Moreover, we obtained
the tidal radius, core radius, and clear evidence of mass segregation in ten
clusters. From an examination of the high-quality color-magnitude data of the
cluster, we obtained one white dwarf for each of NGC752, Coma Ber and M67. In
the young open cluster M38, we found all members inside the tidal radius
however in the older clusters we found some members outside of the tidal
radius, indicating that the young open clusters had not enough time to form
clear tidal tails. It is seen that mass segregation occurs at a higher rate in
older clusters than the younger ones.
