Simulations of Colliding Uniform Density H2 Clouds

Abstract

In this paper we present a set of numerical simulations designed to study the interaction process of H II molecular clouds. For the initial conditions we assume head-on and oblique collisions of binary identical clouds placed adjacent to one another, with their surfaces just in contact. The colliding initial clouds are uniform density molecular gas spheres with rigid body rotation. The cloud initial conditions are chosen to favor its gravitational collapse as an isolated system. To study the effect of the self-gravity of the cloud in the collision process, we consider several models in which the approaching speed of the colliding clouds increases from zero up to several times the initial sound speed of the barotropic gas. We present the outcome of these collision models for several values of the impact parameter b, which depends on the initial radius of the cloud. We have explored the parameter space of the approaching velocity Vapp of the colliding clouds for configurations that may result in seeds for the formation of more complex systems. Such systems are expected to include filaments and gas clumps, where the star formation process is still possible despite the occurrence of the collision. We show hereby that collisions may have a major and favorable influence on the star formation process.

Physical Properties of a Molecular Cloud after a Penetrating Collision

“…The studies performed by [7] and [8] have had an influence in the present paper, as we have attempted to take some of their ideas into account in order to improve their simulations. Besides, the present investigation can be considered as a continuation of the study carried out by [9] (hereafter Paper I). It must be emphasized that collision models of two gas cores, from a purely theoretical perspective with no intention of making any comparison with some observed systems, have been numerically studied in both Paper I and in the present paper.…”

“…In the present study a total set of particles generated the two initial cores by a traditional Monte Carlo scheme, in which the particles are located randomly in the volume space, as has already been previously described by [9].…”

The motion of a relativistic charged particle in a homogenous electromagnetic field in De-Sitter space

“…where θ = η γα DX γ ds DX α ds [1]. This approach has been effectively used to determine the dynamics of a system even though its internal form is not fully solved.…”