| Name: Shubhankar Gharote |
| Affiliation: Space Applications Centre (ISRO) |
| Conference ID: ASI2026_262 |
| Title: Dense Structure Formation in Merging Interstellar Filaments: Hydrodynamic Simulations |
| Abstract Type: Poster |
| Abstract Category: Stars, Interstellar Medium, and Astrochemistry in Milky Way |
| Author(s) and Co-Author(s) with Affiliation: Shubhankar Ravindra Gharote(Space Applications Centre, Ahmedabad - 380015, India), Vibhuti Bhushan Jha(Space Applications Centre, Ahmedabad - 380015, India) |
| Abstract: Filamentary structures are a ubiquitous component of the interstellar medium (ISM) and play a central role in regulating star formation in the Milky Way. These filaments frequently undergo mergers, giving rise to complex filamentary systems, including tuning-fork–like morphologies formed by the interaction of two filaments. While recent studies have established links between hydrodynamic simulations and observations of such structures, the statistical impact of key parameters, such as merger geometry and relative velocities on the properties of the resulting clumps and dense cores remains to be explored.
We perform three-dimensional, self-gravitating hydrodynamic simulations of filament mergers using the adaptive mesh refinement code RAMSES, systematically varying merger geometry and velocity of approach. The filaments are initialized in radial hydrostatic equilibrium with the ambient medium, with axial density gradients introduced to ensure merger prior to end-dominated collapse. Controlled bulk velocities are then imposed to drive filament interactions. The physical properties of the resulting clumps and dense cores are quantified.
We find that increasing the velocity of approach promotes the formation of long-lived dense structures up to a critical velocity, beyond which the merged system becomes gravitationally unbound. Merger geometry significantly influences dense structure properties by regulating the effective volume of the interaction region. We construct a two-dimensional phase diagram of clump and core properties as a function of merger velocity and angle, and discuss the implications for filament evolution. Future studies will focus on the role of turbulence and magnetic field as additional influencing factors in filament mergers. |
