Simulations of un-equal binary collisions embedded in a turbulent gas cloud far away of a massive gravitational center

Abstract

We simulate the collapse of a turbulent gas cloud with the particle-based code Gadget2. We choose two sub-clouds, formed by those particles located around the centers ${\vec{r}}_L$ and ${\vec{r}}_R$ and within the radii $r_L$ and $r_R$, respectively. A translational velocity ${\vec{v}}_L$ or ${\vec{v}}_R$ is added, so that the sub-clouds move towards each other to collide. The radius and pre-collision velocity of the sub-clouds are chosen to be un-equal, and both head-on and oblique collisions are considered. The simulations are all calibrated to have the same total mass and the initial energy ratio $\alpha =0.16$, which is defined as the ratio of thermal energy to gravitational energy. We compare low-$\beta$ models to a high-$\beta$ models, where $\beta$ is defined as the ratio of kinetic energy to gravitational energy. Finally, we consider the turbulent cloud to be under the gravitational influence of an object located far enough, in order to approximate the tidal effects by means of an azimuthal velocity $V_{\mathrm{cir}}$ added to the cloud particles in addition to the translational and turbulent velocities mentioned above. We compare a low-$V_{\mathrm{cir}}$ model with a high-$V_{\mathrm{cir}}$ one.

Accepted for publication in Revista Mexicana de Astronomia y Astrofisica

References in corpus (7)

• The Resolved Properties of Extragalactic Giant Molecular Clouds
• Molecular Cloud Evolution II. From cloud formation to the early stages of star formation in decaying conditions
• The dynamical evolution of molecular clouds near the Galactic Centre - I. Orbital structure and evolutionary timeline
• Do cloud-cloud collisions trigger high-mass star formation? I. Small cloud collisions
• A cluster in the making: ALMA reveals the initial conditions for high-mass cluster formation
• The dynamical evolution of molecular clouds near the Galactic Centre - II. Spatial structure and kinematics of simulated clouds
• The dynamical evolution of molecular clouds near the Galactic Centre -- III. Tidally--induced star formation in protocluster clouds