The Role of Magnetic Fields in Regulating Galaxy Cluster Interactions

Belay Sitotaw Goshu

Abstract


Witness the universe evolve in real-time through interactions with galaxy clusters, and colossal structures. In this work, we aim to explore the role of energy distribution and density in disturbed galaxy clusters. The study evolution of energy and density in two-dimensional systems using large-scale numerical simulations. The continuity, momentum, and energy equations were solved in a finite difference time domain to employ magnetic and gravitational fields. The results show that the density distribution is highest in the core and peaks at radii external to this, within galaxy clusters. Meanwhile, the energy density is shown to be reduced at the core and maxima radially outwards where it reaches a maximum around the outer limit of densities. This correlation shows how this gradient in the density modifies its energy distribution. These findings are consistent with prior simulation studies and theoretical models. In conclusion, understanding the dynamics and evolution of galaxy clusters requires understanding density patterns and energy distribution.  More intricate simulations involving extra physical processes like dark matter interactions and magnetic fields should be a part of future efforts.


Keywords


Galaxy clusters, finite difference time domain approach perturbation, density distribution, energy density, and numerical simulations

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References


Brandenburg, A., & Subramanian, K. (2005). Astrophysical magnetic fields and nonlinear dynamo theory, Physics Reports, 417(1-4), 1-209.

Brüggen, M., & Kaiser, C. R. (2001). Magnetic Fields in Galaxy Clusters: Observations and Theoretical Models, Monthly Notices of the Royal Astronomical Society, 325(2), 676–682.

Brunetti, G. & Jones, T. W. (2014). Cosmic rays in galaxy clusters and their nonthermal emission. International Journal of Modern Physics D, 23(04), 1430007.

Carilli, C. L., & Taylor, G. B. (2002). Cluster Magnetic Fields Annual Review of Astronomy and Astrophysics, 40, 319–348.

Chandrasekhar, S. (1961). Hydrodynamic and hydromagnetic stability Clarendon Press.

Dolag, K., & Stasyszyn, F. (2009). An MHD gadget for cosmological simulations, Monthly Notices of the Royal Astronomical Society, 398(4), 1678–1697.

Dolag, K., Bartelmann, M., & Lesch, H. (2002). SPH simulations of magnetic fields in galaxy clusters. Astronomy & Astrophysics, 387(2), 383-395.

Dolag, K., Grasso, D., Springel, V., & Tkachev, I. (2005). Constrained Simulations of the Magnetic Field in the Local Universe and the Propagation of UHECRs, Journal of Cosmology and Astroparticle Physics, 2005 (01), 009.

Fabian, A. C. (2012). Observational Evidence of AGN Feedback, Annual Review of Astronomy and Astrophysics, 50, 455–489.

Feretti, L., Giovannini, G., Govoni, F., & Murgia, M. (2012). Clusters of galaxies: observational properties of the diffuse radio emission, Astronomy & Astrophysics Review, 20, 54.

Gianfagna, G., & Teyssier, R. (2018). Gravitational collapse of the most massive halos in the universe. Monthly Notices of the Royal Astronomical Society, 476(4), 476-490.

Govoni, F. & Feretti, L. (2004). Magnetic fields in clusters of galaxies. International Journal of Modern Physics D, 13(08), 1549-1594.

Krumholz, M. R., & Federrath, C. (2019). The Role of Magnetic Fields in the Star Formation Process. Frontiers in Astronomy and Space Sciences, 6, 7.

Kulsrud, R. M. (2005). Plasma Physics for Astrophysics, Princeton University Press.

Markevitch, M. & Vikhlinin, A. (2007). Shocks and cold fronts in galaxy clusters. Physics Reports, 443(1-2), 1-53.

Parrish, I. J., Quataert, E., & Sharma, P. (2012). Inhibition of thermal conduction by tangled magnetic fields in clusters of galaxies. The Astrophysical Journal, 703(1), 96-107.

Poole, G. B., et al. (2006). "Evolution of Cluster Cores and Scaling Relations in Numerical Simulations of Galaxy Cluster Mergers." The Astrophysical Journal, 639(2), 590–615.

Ricker, P. M., & Sarazin, C. L. (2001). "Heating and Cooling of the Intracluster Medium by Cluster Mergers, The Astrophysical Journal, 561(2), 621-644.

Ryu, D., Kang, H., Cho, J., & Das, S. (2008). Turbulence and Magnetic Fields in the Large-Scale Structure of the Universe. Science, 320 (5878), 909–912.

Sarazin, C. L. (1988). X-ray emission from clusters of galaxies. Cambridge University Press.

Springel, V., Yoshida, N., & White, S. D. M. (2001). GADGET: A code for collisionless and gas dynamical cosmological simulations. New Astronomy, 6(2), 79–117.

Stone, J. M., Gardiner, T. A., Teuben, P., Hawley, J. F., & Simon, J. B. (2008). Athena: A new code for astrophysical MHD. The Astrophysical Journal Supplement Series, 178(1), 137–177.

Subramanian, K., Shukurov, A., & Haugen, N. E. L. (2006). Evolving Turbulence and Magnetic Fields in Galaxy Clusters. Monthly Notices of the Royal Astronomical Society, 366(4), 1437–1454.

Vogelsberger, M., et al. (2012), A model for cosmological simulations of galaxy formation physics, Monthly Notices of the Royal Astronomical Society, 425(4), 3024–3057.

Xu, H., Li, H., Collins, D. C., Li, S., & Norman, M. L. (2019), The impact of magnetic fields on the evolution of galaxy clusters, The Astrophysical Journal, 885(2), 162.

ZuHone, J. A., et al. (2010), AGN Feedback and the Role of Cluster Merger Dynamics in the Gas Heating of Galaxy Clusters, The Astrophysical Journal, 716(2), 909–927.




DOI: https://doi.org/10.33258/birex.v6i4.8003

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