Ursprung und Effekt von kosmischer Strahlung in kosmologischen Strukturen
Zusammenfassung der Projektergebnisse
In this project, Mr Wittor analysed simulations performed with a cosmological magnetohydrodynamics code to study the non-thermal components of the intracluster medium. In particular, he has written a code that follows fluid particles in a Lagrangian fashion in post-processing. He then employed this code to study the radio emission at shock waves that occur when galaxy clusters merge. We performed an extensive study to verify whether the obliquity of the magnetic field at the shock wave has an effect on the radio emission observed at radio relics and the abundance of cosmic ray protons in the intracluster medium. Finally, we studied the evolution of vorticity and enstrophy in the intracluster medium. This work was done in collaboration with Prof. Tom Jones at the University of Minnesota and contains very interesting results on the nature of the turbulence and the timescales involved. For example, it was shown that mainly stretching motions in the gas are responsible for the evolution of enstrophy (and thus turbulence). This work will have a great impact on attempts to derive estimates of turbulent pressures from X-ray observations. It was also shown how the dissipation of turbulence can explain the observed magnetic field strengths in galaxy clusters. Thus, this very theoretical piece of work has made very tangible connections to observable quantities.
Projektbezogene Publikationen (Auswahl)
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2016, Galaxies, 4, 71
Wittor, D., Vazza, F., & Brüggen, M.
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2016, MNRAS , 459, 70
Vazza, F., Brüggen, M., Wittor, D., et al.
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2017, Classical and Quantum Gravity, 34, 234001
Vazza, F., Brüggen, M., Gheller, C., et al.
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2017, MNRAS , 464, 4448
Wittor, D., Vazza, F., & Brüggen, M.
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2017, MNRAS , 471, 3212
Wittor, D., Jones, T., Vazza, F., & Brüggen, M.
