Star Formation Triggered by Shocks

Star formation can be triggered by compression from shock waves. In this study, we investigated the interaction of hydrodynamic shocks with Bonnor–Ebert spheres using 3D hydrodynamical simulations self-gravity. Our indicated that cloud evolution primarily depends on two parameters: speed and initial radius. Stronger compress clouds more efficiently, when central region becomes gravitationally unstable, a triggers contraction. However, if it is excessively strong, shreds violently destroyed. From simple theoretical considerations, derived condition gravitational collapse, which agreed simulation results. Introducing sink particles, followed further after star formation. Since stronger tend to shred material is, smaller final (asymptotic) masses stars formed (i.e., particles) become. addition, accelerate clouds, promoting mixing shock-accelerated interstellar medium gas. As result, separation between particles shocked center their relative speeds increase over time. We also effect turbulence shock–cloud interaction. observed prevents rapid contraction; thus, turbulent are destroyed rapidly than thermally supported clouds. Therefore, become smaller. provide general guide evolutionary process dense cores Bok globules impacted shocks.