The properties of magnetised cold filaments in a cool-core galaxy cluster

被引:2
|
作者
Fournier, M. [1 ]
Grete, P. [1 ]
Brueggen, M. [1 ]
Glines, F. W. [2 ,3 ]
O'Shea, B. W. [2 ,3 ,4 ]
机构
[1] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany
[2] Michigan State Univ, Dept Computat Math Sci & Engn, E Lansing, MI 48824 USA
[3] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA
[4] Michigan State Univ, Facil Rare Isotope Beams, E Lansing, MI 48824 USA
关键词
galaxies: clusters: intracluster medium; galaxies: jets; galaxies: magnetic fields; large-scale structure of Universe; H-ALPHA FILAMENTS; GALACTIC NUCLEUS FEEDBACK; COSMIC-RAY FEEDBACK; INTRACLUSTER MEDIUM; PERSEUS CLUSTER; MOLECULAR GAS; SURFACE BRIGHTNESS; AGN FEEDBACK; HOT GAS; FLOWS;
D O I
10.1051/0004-6361/202451031
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Context. Filaments of cold gas (T <= 104 K) are found in the inner regions of many cool-core clusters. These structures are thought to play a major role in the regulation of feedback from active galactic nuclei (AGNs). Aims. We study the morphology of the filaments, their formation, and their impact on the propagation of the outflowing AGN jets. Methods. We present a set of GPU-accelerated 3D magnetohydrodynamic simulations of an idealised Perseus-like cluster using the performance portable code ATHENAPK. We include radiative cooling and a self-regulated AGN feedback model that redistributes accreted material through kinetic, thermal, and magnetic feedback. Results We confirm that magnetic fields play an important role in both the formation and evolution of the cold material. These suppress the formation of massive cold discs and favour magnetically supported filaments over clumpy structures. Achieving resolutions of 25 - 50 pc, we find that filaments are not monolithic as they contain numerous and complex magnetically supported sub-structures. We find that the mass distribution of these clumps follows a power law of slope of similar to - 0.6 for all investigated filaments. Studying the evolution of individual filaments, we find that their formation pathways can be diverse. We find examples of filaments forming through a combination of gas uplifting and condensation, as well as systems of purely infalling clumps condensing out of the intracluster medium. The density contrast between the cold gas and the outflowing hot material leads to recurring deflections of the jets, favouring inflation of bubbles. Conslusions. Filaments in cool-core clusters are clumpy and contain numerous sub-structures, resulting from a complex interplay between magnetic fields, thermal instability, and jet-cloud interaction. Frequent deflections of the AGN outflows suppress jet collimation and favour the formation of large X-ray bubbles, and smaller off-axis cavities.
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页数:19
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