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The Universe is pervaded by magnetic fields in different scales, although forsimplicity, they are ignored in most cosmological simulations. In this paper,we use the TNG50, which is a large cosmological galaxy formation simulationthat incorporates magnetic fields with an unprecedented resolution. We studythe correlation of the magnetic field with various galaxy properties such asthe total, stellar and gaseous mass, circular velocity, size and star formationrate. We find a linear correlation between the average magnetic field pervadingthe disc of galaxies in relative isolation and their circular velocities. Inaddition we observed that in this sample the average magnetic field in the discis correlated with the total mass as $\overline{B}\simM_{\mathrm{tot,\,R_{\star}}}^{0.2}$. We also find that the massive galaxieswith active wind-driven black hole feedback, do not follow this trend, as theirmagnetic field is substantially affected by this feedback mode in the TNG50simulation. We show that the correlation of the magnetic field with the starformation rate is a little weaker than the circular velocity. Moreover, wecompare the magnetic field components of the above sample with a compiledobservational sample of non-cluster non-interacting nearby galaxies. Similar tothe observation, we find a coupling between the ordered magnetic field and thecircular velocity of the flat part of the rotation curve in the simulation,although contrary to the observation, the ordered component is dominant in thesimulation.

Reconciling the magnetic field in central disc galaxies with the dynamical mass using the cosmological simulations