The winds of young Solar-type stars in the Pleiades, AB Doradus, Columba and $\beta$ Pictoris

Abstract

Solar-type stars, which shed angular momentum via magnetised stellar winds, enter the main sequence with a wide range of rotational periods $P_{\text{rot}}$. This initially wide range of rotational periods contracts and has mostly vanished by a stellar age $t\sim 0.6$ Gyr, after which Solar-type stars spin according to the Skumanich relation $P_{\text{rot}}\propto \sqrt{t}$. Magnetohydrodynamic stellar wind models can improve our understanding of this convergence of rotation periods. We present wind models of fifteen young Solar-type stars aged from 24 Myr to 0.13 Gyr. With our previous wind models of stars aged 0.26 Gyr and 0.6 Gyr we obtain thirty consistent three-dimensional wind models of stars mapped with Zeeman-Doppler imaging - the largest such set to date. The models provide good cover of the pre-Skumanich phase of stellar spin-down in terms of rotation, magnetic field, and age. We find that the mass loss rate $\dot{M}\propto {\Phi }^{0.9\pm 0.1}$ with a residual spread of 150% and that the wind angular momentum loss rate $\dot{J}\propto P_{\text{rot}}^{-1}{\Phi }^{1.3\pm 0.2}$ with a residual spread of 500% where $\Phi$ is the unsigned surface magnetic flux. When comparing different magnetic field scalings for each single star we find a gradual reduction in the power-law exponent with increasing magnetic field strength.

arXiv comment19 pages, 7 figures

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