The nature of the dynamo in the very late M dwarf stars
The results demonstrate that there are non-dMe stars with spectral types later than M5.5. We also confirm the occurrence of dMe stars at very late spectral types that, on the basis of current models, correspond to fully convective interiors. Hence, the results support a rotation-dependent distributed dynamo (or some variation thereof) as a viable model for the generation of magnetic flux in the very low mass stars. Future work should include v sin i determinations in order to further extend the investigation of the properties of dynamos, the kinematics, and the occurrence of binaries in the very low mass stars. The acquisition of Ca II H and K line data for the old disk and halo population stars in order to verify if any chromospheric activity is at all present would prove valuable. Many of the known low luminosity M dwarfs should be targeted for observation with future X-ray satellite observatories. A monitoring program to determine whether cycles occur in the fully convective M dwarf stars would provide valuable input on the location of dynamo processes in the stellar interior, as suggested by Dr. P. Gilman during the course of this workshop.
KeywordsDynamo Model Main Sequence Star Dwarf Star Stellar Interior Chromospheric Activity
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