Our Universe, more specifically, the warm-hot intergalactic medium in the cosmic web filaments, the intra-cluster medium of galaxy clusters, and the circum-galactic medium around individual galaxies is full of such metals. By studying the medium of these massive astrophysical objects through spectroscopy, and by studying the impact of different feedback processes on the metal transport on various physical scales, we can get closer to the understanding of the origin and evolution of metals in some of the most massive objects in our Universe. In this talk I will give an overview of my Ph.D. thesis, which focused on the spectroscopy of the cosmic web (filaments and galaxy clusters) with current and future X-ray telescopes like e.g. NewAthena. I will show that future X-ray micro-calorimeter missions will be sensitive to effects that have not yet been detected before, like for example observing WHIM in absorption against bright cool-core clusters. I will briefly mention the importance of updating the atomic databases and plasma codes in the X-ray regime. In the past two years, I shifted my career towards the space industry, more specifically, over time I got more involved in the QUVIK mission - the very first Czech-led space telescope for which I recently accepted a role of the main project manager. I will briefly mention updates about QUVIK. I will also briefly talk about the new science public outreach activities that we are preparing in Brno together with my colleagues.

Location: ASU Spořilov, 101

Magnetised bubbles pervade the interstellar medium across a vast range of scales, from individual supernova remnants (SNRs) to the superbubbles they collectively inflate. We present two complementary 3D magnetohydrodynamic studies tracing this hierarchy from its smallest building blocks to its most prominent local example. We simulate SNRs expanding into a non-homogeneous, magnetised two-phase medium, obtaining complex magnetic field configurations in their interiors. Strongly magnetised remnants develop magnetically confined hot cavities surrounded by a diffuse magnetised halo, and remain orders of magnitude more X-ray luminous than their weakly magnetised counterparts. We then extend our study to larger scales, simulating the Local Bubble: a superbubble encasing the Solar neighbourhood, whose expansion has been driven by numerous supernovae. We characterise its turbulent interior magnetic field and its amplification in the shell, while also modelling neighbouring superbubbles and SNRs within 1 kpc of the Sun. Together, these parsec- to kiloparsec-scale frameworks give us insights on the coupling between magnetic fields and stellar feedback, from individual remnants to the large-scale cavities structuring the local interstellar medium.

Location: Spořilov - Lecture Room 101