The impact of magnetic fields on cosmological galaxy mergers - II. Modified angular momentum transport and feedback

被引:6
|
作者
Whittingham, Joseph [1 ,2 ]
Sparre, Martin [1 ,2 ]
Pfrommer, Christoph [1 ]
Pakmor, Ruediger [3 ]
机构
[1] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany
[2] Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany
[3] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany
基金
欧洲研究理事会;
关键词
MHD; methods: numerical; galaxies: interactions; galaxies: magnetic fields; MOVING-MESH COSMOLOGY; SMOOTHED PARTICLE HYDRODYNAMICS; STAR-FORMATION; DISC GALAXIES; CIRCUMGALACTIC MEDIUM; ILLUSTRIS PROJECT; SECULAR EVOLUTION; PULSAR ROTATION; BARRED GALAXIES; SIMULATIONS;
D O I
10.1093/mnras/stad2680
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The role of magnetic fields in galaxy evolution is still an unsolved question in astrophysics. We have previously shown that magnetic fields play a crucial role in major mergers between disc galaxies; in hydrodynamic simulations of such mergers, the Auriga model produces compact remnants with a distinctive bar and ring morphology. In contrast, in magnetohydrodynamic (MHD) simulations, remnants form radially extended discs with prominent spiral arm structure. In this paper, we analyse a series of cosmological 'zoom-in' simulations of major mergers and identify exactly how magnetic fields are able to alter the outcome of the merger. We find that magnetic fields modify the transport of angular momentum, systematically hastening the merger progress. The impact of this altered transport depends on the orientation of the field, with a predominantly non-azimuthal (azimuthal) orientation increasing the central baryonic concentration (providing support against collapse). Both effects act to suppress an otherwise existent bar-instability, which in turn leads to a fundamentally different morphology and manifestation of feedback. We note, in particular, that stellar feedback is substantially less influential in MHD simulations, which allows for the later accretion of higher angular momentum gas and the subsequent rapid radial growth of the remnant disc. A corollary of the increased baryonic concentration in MHD simulations is that black holes are able to grow twice as large, although this turns out to have little impact on the remnant's development. Our results show that galaxy evolution cannot be modelled correctly without including magnetic fields.
引用
收藏
页码:224 / 245
页数:22
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