Efficient cosmic-ray transport in CR-pressure-dominated CGM simulations produces stronger cool-gas absorption (MgII, SiII) and covering fractions matching star-forming galaxies, while slow transport underproduces them.
Simulations of magnetic fields in isolated disk galaxies
6 Pith papers cite this work. Polarity classification is still indexing.
6
Pith papers citing it
abstract
Magnetic fields are known to be dynamically important in the interstellar medium of our own Galaxy, and they are ubiquitously observed in diffuse gas in the halos of galaxies and galaxy clusters. Yet, magnetic fields have typically been neglected in studies of the formation of galaxies, leaving their global influence on galaxy formation largely unclear. We extend our MHD implementation in the moving-mesh code Arepo to cosmological problems which include radiative cooling and the formation of stars. In particular, we replace our previously employed divergence cleaning approach with a Powell 8-wave scheme, which turns out to be significantly more stable, even in very dynamic environments. We verify the improved accuracy through simulations of the MRI in accretion disks, that reproduce its correct linear growth rate. Using this new MHD code, we simulate the formation of isolated disk galaxies similar to the Milky Way using idealized initial conditions with and without magnetic fields. We find that the magnetic field is quickly amplified in the initial starburst and the differential rotation of the forming disk until it eventually saturates when it becomes comparable to the thermal pressure. The additional pressure component leads to a lower star formation rate at late times compared to simulations without magnetic fields, and induces changes in the spiral arm structures of the gas disk. In addition, we observe highly magnetized fountain-like outflows from the disk. These results are robust with numerical resolution and are largely independent of the initial magnetic seed field assumed in the initial conditions, as the amplification process is rapid and self-regulated. Our findings suggest an important influence of magnetic fields on galaxy formation and evolution, cautioning against their neglect in theoretical models of structure formation.
years
2026 6representative citing papers
A CNN trained on AREPO simulations and synthetic observations reverts edge-on 13CO spectral data to top-down views of the CMZ as a proof-of-concept for supervised reversion.
TNG100 and EAGLE hydrodynamical simulations underproduce faint compact galaxies at z>3 relative to CANDELS observations even after forward modeling and completeness corrections, with the mismatch linked to both detection effects and simulation physics.
50 constrained simulations of Coma cluster analogues reproduce the observed radial X-ray surface brightness and Compton-y profiles within the scatter expected from environment and assembly history.
Proposes SKA surveys for a census of galactic magnetic fields from low to high redshift using polarimetry, RM grids, and lensed quasars to constrain dynamo models.
Review chapter summarizing the importance of small-scale galactic magnetic fields and proposing SKA observation strategies.
citing papers explorer
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CRexit observed: probing cosmic ray transport in the circumgalactic medium with absorption line spectra
Efficient cosmic-ray transport in CR-pressure-dominated CGM simulations produces stronger cool-gas absorption (MgII, SiII) and covering fractions matching star-forming galaxies, while slow transport underproduces them.
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IRIS: Deciphering Spectral-Line Imagery of the Galactic Center by Machine-Learning on Simulations
A CNN trained on AREPO simulations and synthetic observations reverts edge-on 13CO spectral data to top-down views of the CMZ as a proof-of-concept for supervised reversion.
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Probing the faint end of simulated galaxy counts at z>3
TNG100 and EAGLE hydrodynamical simulations underproduce faint compact galaxies at z>3 relative to CANDELS observations even after forward modeling and completeness corrections, with the mismatch linked to both detection effects and simulation physics.
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Learning the Universe: Constrained simulations of the Coma galaxy cluster -- I. Radial X-ray and Compton-y signatures
50 constrained simulations of Coma cluster analogues reproduce the observed radial X-ray surface brightness and Compton-y profiles within the scatter expected from environment and assembly history.
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Probing Magnetic Fields In and Around Galaxies Near and Far
Proposes SKA surveys for a census of galactic magnetic fields from low to high redshift using polarimetry, RM grids, and lensed quasars to constrain dynamo models.
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Small-scale Magnetic Fields in the Milky Way and Nearby Galaxies
Review chapter summarizing the importance of small-scale galactic magnetic fields and proposing SKA observation strategies.