Open clusters (OCs) provide a controlled setting to investigate the interplay between mass and metallicity on a more localized level. However, the specific analysis of this relation within individual open clusters has been sparsely investigated, despite its significance.
In this study, we aim to fill this research gap by conducting a comprehensive analysis of 100-star clusters, with the objective of examining the trends and probing the underlying mechanisms governing their mass-metallicity relationship. To achieve this objective, we utilize the Gaia Data Release 3 (DR3) dataset, which offers precise astrometric and photometric measurements for a vast number of celestial objects. Additionally, we used APSIS dataset to access the mass and metallicity of individual stars. The membership of stars within each cluster is confirmed using the HDBScan algorithm, ensuring the accuracy of our analysis. We employ a power-law model to fit the mass-metallicity relation mostly in the domain of 0.6 M☉< M <1.4 M☉, and determine the nature of the observed trend. Furthermore, we fit isochorones in the HR diagram to determine the age and metallicities of the OCs. Our initial results reveal a pattern among the star clusters studied: approximately 70% of them exhibit a distinct negative power-law relationship(γ). This implies that as the mass of stars increases in the OCs, their metallicity tends to decrease. However, further investigation is required to validate and expand upon this observation.