Research: Rotation and activity in early- to mid-type M-stars
Stellar rotation, the very cause of the generation of magnetic field, induces activity in the stars. This type of rotation-activity relation has been found sustainable for the stars with outer convective envelope. The vigor of this relation is clear for the solar-type stars, but for the stars with deeper outer convective layer or for the fully-convective stars, the clarity of this relation becomes feeble. The main reason has been that the rotational braking, defined by Skumanich, for main-sequence stars found to be inconsistent for fully-convective stars. Therefore, my main objective is to study the sample of stars in the spectral regime from early- to mid-type M-dwarfs for rotation-activity relation. This spectral regime coincides with the mass range for main sequence stars describing the transition from partial to full convection. This research project shall shed more light on whether the rotation-activity relation is consistent with the stars obeying different rotational braking mechanism.