The theoretical instability strip of M dwarf stars

The overstability of the fundamental radial mode inMdwarf modelswas theoretically predicted recently by Rodríguez-López et al. The periods were found to be in the ranges ̃25-40 min and ̃4-8 h, depending on stellar age and excitation mechanism.We have extended our initial Mdwarf model grid in mass, metallicity and mixing length parameter.We have also considered models with boundary conditions from PHOENIX NEXTGEN atmospheres to test their influence on the pulsation spectra.We find instability of non-radial modes with radial orders up to k = 3, degree l = 0-3, including p-and g-modes, with the period range extending from 20 min up to 11 h. Furthermore, we find theoretical evidence of the potential of M dwarfs as solar-like oscillators. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.