<p>In this study, we present our scientific approach to observationally infer possible correlations of the disruption age with the stellar surface density and two-dimensional radius for 200 open star clusters within the solar neighbourhood. A detailed statistical analysis of number density, core and tidal radius, mass, and log(age) has also been presented using the Gaia EDR3 database. The initial mass and disruption time of the individual clusters are calculated using the analytical relations available in the literature, considering the cluster mass loss mechanism due to stellar evolution and tidal interactions. Considering the mass loss models used in this study, we also observe the variation of the initial mass of the star clusters as a function of their present age. We carry out a linear fit for the variation of the cluster disruption time with its number density, which gives an approximate correlation of the form, <InlineEquation ID="IEq1"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10101_Article_IEq1.gif" Format="GIF" Height="20" Rendition="HTML" Resolution="72" Type="Linedraw" Width="117" /> </InlineMediaObject> <EquationSource Format="TEX">\(t_{\textrm{dis}}\propto \rho _{o}^{0.230\pm 0.052}\)</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <msub> <mi>t</mi> <mtext>dis</mtext> </msub> <mo>∝</mo> <msubsup> <mi>ρ</mi> <mrow> <mi>o</mi> </mrow> <mrow> <mn>0.230</mn> <mo>±</mo> <mn>0.052</mn> </mrow> </msubsup> </mrow> </math></EquationSource> </InlineEquation>. We also assess this linear relation using statistical correlations, which results in a moderate coefficient value of 0.3903. This statistical correlation and the power law relation illustrate that disruption time increases with the increasing stellar surface density of the cluster. We also observationally and statistically investigate the correlation between the radius and disruption time of the clusters, but no prominent dependence was found between them.</p>