| Name: Pranaav S |
| Affiliation: Manipal Center for Natural Sciences, MAHE |
| Conference ID: ASI2026_504 |
| Title: Magnetic Field Evolution in Cosmic Web Nodes |
| Abstract Type: Poster |
| Abstract Category: Galaxies and Cosmology |
| Author(s) and Co-Author(s) with Affiliation: Pranaav S(Manipal Center for Natural Sciences, Manipal - 576104, India), Surajit Paul(Manipal Center for Natural Sciences, Manipal - 576104, India) |
| Abstract: The most massive gravitationally bound structures in the Universe are galaxy clusters, which reside at the nodes of the cosmic web. Early dark matter simulations revealed the structure of the cosmic web, but a purely gravitational description is fundamentally incomplete. The presence of baryonic matter in the form of tenuous astrophysical plasma composed of charged particles provides a compelling argument for the existence of magnetic fields in the intracluster medium (ICM). This is further supported by observations indicating microgauss-level magnetic fields in cluster environments. Our understanding of magnetic field amplification and evolution in large-scale structures remains incomplete, as existing studies have focused on limited samples of galaxy clusters, and the spatial and temporal evolution of magnetic fields has not been explored extensively.
At present, due to the limited availability of observational data, the study of cosmic magnetic fields—particularly their physical origin and evolution—remains highly challenging. However, recent advances in high-resolution cosmological magnetohydrodynamic (MHD) simulations that aim to realistically model physical processes, such as the IllustrisTNG suite of high-resolution MHD simulations, offer new insights. In this study, we implement a physically robust classification of clusters based on their dynamical state using a combination of physically relevant parameters including but not limited to merger mass ratio (ε), Relaxation period (t), Centroid shift (ω) and Virial ratio (η) on a statistically significant sample of galaxy clusters in TNG-Cluster simulation. We analyze their magnetic properties by employing Triangular-Shaped Cloud algorithm to offset Voronoi mesh structure of IllustrisTNG. The analyzed data is further tested for magnetic field amplification mechanisms - Adiabatic compression and models of turbulent dynamo to validate the z = 0 magnetic field of ICM, In this conference we will be presenting the preliminary results of this study. |
