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.

arXiv commentAccepted for publication in Revista Mexicana de Astronomia y Astrofisica

References in corpus (19)

• 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
• A 100-parsec elliptical and twisted ring of cold and dense molecular clouds revealed by Herschel around the Galactic Center
• Variations in the Galactic star formation rate and density thresholds for star formation
• Low Virial Parameters in Molecular Clouds: Implications for High Mass Star Formation and Magnetic Fields
• The dynamical evolution of molecular clouds near the Galactic Centre - I. Orbital structure and evolutionary timeline
• Tidal Effects in Clusters of Galaxies
• Tidal Shocking by Extended Mass Distributions
• Do cloud-cloud collisions trigger high-mass star formation? I. Small cloud collisions
• Simulating star formation in molecular cores II. The effects of different levels of turbulence
• A cluster in the making: ALMA reveals the initial conditions for high-mass cluster formation
• Star formation in clusters: early sub-clustering in the Serpens core
• The dynamical evolution of molecular clouds near the Galactic Centre - II. Spatial structure and kinematics of simulated clouds
• Formation of star clusters in the LMC and SMC. I. Preliminary results on cluster formation from colliding gas clouds
• Gravity or turbulence? IV. Collapsing cores in out-of-virial disguise
• The dynamical evolution of molecular clouds near the Galactic Centre -- III. Tidally--induced star formation in protocluster clouds
• Supersonic Cloud Collision - I
• The Inevitable Future of the Starless Core Barnard 68
• Supersonic Cloud Collision-II