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Star formation has been observed to occur at globally low yet locally varyingefficiencies. As such, accurate capture of star formation in numericalsimulations requires mechanisms that can replicate both its smaller-scalevariations and larger-scale properties. Magnetic fields are thought to play anessential role within the turbulent interstellar medium (ISM) and affectmolecular cloud collapse. However, it remains to be fully explored how amagnetised model of star formation might influence galaxy evolution. We presenta new model for a sub-grid star formation recipe that depends on the magneticfield. We run isolated disk galaxy simulations to assess its impact on theregulation of star formation using the code RAMSES. Building upon existingnumerical methods, our model derives the star formation efficiency from localproperties of the sub-grid magnetised ISM turbulence, assuming a constantAlfv\'en speed at sub-parsec scales. Compared to its non-magnetisedcounterpart, our star formation model suppresses the initial starburst by afactor of two, while regulating star formation later on to a nearly constantrate of $\sim 1~M_{\odot}~\mathrm{yr}^{-1}$. Differences also arise in thelocal Schmidt law with a shallower power law index for the magnetised starformation model. Our results encourage further examination into the notion thatmagnetic fields are likely to play a non-trivial role in our understanding ofstar and galaxy formation.

A new star formation recipe for magneto-hydrodynamics simulations of galaxy formation