Abstract
In the present paper we try to reproduce the observed dependence of rotation decay of main sequence stars in the mass range 1.1–0.5 M⊙. We adopt a radial magnetic field structure which yields the t-1/2 relation and the observed magnetic field values as given by Saar(1990). We assume that the effective magnetic field at photospheric level is given by the product of the equipartition field B eq by the filling factor f, and that the latter is proportional to the angular rotation ω. The results are consistent with the observed rotation rate decay as a function of the mass and do suggest that the whole star is slowed down.
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Trigilio, C., Umana, G., Catalano, S., Marilli, E. (1991). The Spin-Down of Main Sequence Stars Based on Observed Magnetic Field Strength. In: Catalano, S., Stauffer, J.R. (eds) Angular Momentum Evolution of Young Stars. NATO ASI Series, vol 340. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-3580-1_33
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DOI: https://doi.org/10.1007/978-94-011-3580-1_33
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