We report the tidal disruption of very low–mass stars (VLMS) by a $100\,M_{\odot }$ black hole (BH) using five hydrodynamical models (M1–M5) with stellar masses of 0.08, 0.16, 0.24, 0.32, 0.40 $M_{\odot }$ and radii of 0.132, 0.230, 0.319, 0.401, 0.480 $R_{\odot }$ , respectively. Although all stars begin from the same initial position, their dynamical evolution diverges rapidly as they approach pericenter. The lowest–mass star (M1) undergoes the strongest early deformation due to its weak self–gravity, while higher–mass stars remain more structurally coherent. Surface–density maps show that massive stars retain dense cores after disruption, whereas lower–mass stars become more fully stretched and stripped. All models exhibit a sharp reduction in bound mass near pericenter, marking the moment when tidal forces exceed stellar self–gravity. M1 retains the least post–pericenter mass, while M4 and M5 preserve the largest fraction of their initial mass. Mass–loss histories indicate that M1 experiences the greatest fractional loss, whereas M5 loses the largest absolute amount of material ( $\sim 0.027$ $M_{\odot }$ ). Mass loss becomes efficient once the star crosses its tidal radius, after which all curves plateau as the remnant recedes. Debris morphology depends strongly on stellar mass and the compactness. Also, the bound debris to BH increases from 0.0409 $M_{\odot }$ for the least massive star to 0.2064 $M_{\odot }$ for the most massive one, reflecting the deeper gravitational potential and broader energy spread of more compact stars during tidal disruption. Overall, the results show that stellar compactness governs tidal deformation, mass loss, and debris structure in VLMS tidal disruption events (TDEs).
