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Observation of solar-like stars show a clear relation between X-ray emissionand their rotation. Higher stellar rotation can lead to a larger magnetichelicity production in stars. We aim to understand the relation betweenmagnetic helicity on the surface of a star to their coronal X-ray emission. Weuse 3D MHD simulations to model the corona of the solar-like stars. We take anobserved magnetogram as in photospheric activity input, and inject differentvalues of magnetic helicity. We use synthesis emission to calculate the X-rayemission flux of each simulation and investigate how this scales with injectedmagnetic helicity. We find that for larger injected magnetic helicities anincrease in temperature and an increase in X-ray emission. The X-ray emissionscaled cubicly with the injected helicity. We can related this to increase ofhorizontal magnetic field and therefore higher Poynting flux at the coronalbase. Using typical scaling of magnetic helicity production with stellarrotation, we can explain the increase of X-ray emission with rotation only byan increase of magnetic helicity at the surface of a star.

On the influence of magnetic helicity on X-rays emission of solar and stellar coronae