Abstract Details
| Name: PRATEEK GUPTA Affiliation: S. P . PUNE UNIVERSITY, PUNE, MAHARASHTRA Conference ID: ASI2018_768 Title : Numerical modeling of synchrotron radio emission from large scale structures Authors and Co-Authors : Surajit Paul, Dept of Physics, University of Pune (SPPU), Pune. Reju Sam John, P.E.C., Pondicherry University, Puducherry. Abstract Type : Poster Abstract Category : General Relativity and Cosmology Abstract : In hierarchical structure formation, at large scale (>= 10 Mpc) the Universe comprises of complex filamentary structure in which galaxy clusters, filaments, and voids are its major components. Filaments play the major role, eaten up the matter from voids and feed it to their respective galaxy clusters (knots, created at the junction of filaments). Most of the baryonic matter first processed in filaments and then fed to the hot furnace (galaxy cluster) which in gives out the wealth of information (electromagnetic or particle radiation) about the energetics and processes taken place in the system. The kinetic energy released during structure formation dissipates in the intra-cluster-medium (ICM) by shock thermalization and turbulence generation. The cluster merger and accretion of matter during the structure formation results in the shock waves and fluid turbulence in ICM. These shock waves accelerate the significant population of charged particles of the ICM by diffusive shock acceleration (DSA) mechanism. The fluid turbulence produces the Alfven waves which re-accelerates (turbulence re-acceleration (TRA) mechanism) the existing non-thermal electrons to GeV and also amplifies existing cluster magnetic fields by dynamo action, causing the GeV electrons to efficiently lose energy to synchrotron radiation in the GHz band. This synchrotron radio emission could help in tracing back the dynamical history of these structures. In this work, we deployed both of our particle acceleration model (DSA and TRA) for computing synchrotron radio emission from Large Scale Structures (LSS) using Adaptive Mesh Refinement (AMR), grid-based hybrid (N-body + Hydrodynamical) cosmological simulations. Computation is being done on grid parameters and a proper weight has been used to nullify the effect of complicated resolution pattern of an AMR simulation. Finally, we have created the synthetic radio maps, for each above-stated model and also with combining both models. It explained the observed radio relics found at few Megaparsec away from Galaxy cluster as well as predicted some very interesting radio structures, radio halos, and the existence of the complex filamentary network. In work of ours, we also prepared a catalogue of galaxy clusters and groups having the mass range between 10^13 - few 10^15 Solar mass and computed their corresponding radio power and radio flux using above-stated models and clearly predicted the possible detectable sources with the upcoming radio telescope (SKA). |