Speaker
Matthew Browning
(University of Exeter)
Description
Most stars in our galaxy are smaller than the Sun. More than half (by number) are
M-dwarfs, stars less than half as massive as the Sun and ten to a thousand times less
luminous; below about spectral type M3.5, these stars are convective throughout their
interiors. We examine the differential rotation and magnetism that may be realised
in such stars, using 3-D MHD simulations with the Anelastic Spherical Harmonic (ASH)
code. Our models capture the convective flows within a rotating spherical geometry,
intended to model low mass stars at a range of rotation rates. We focus here on the
interplay between the sustained zonal flows and the dynamo-generated magnetism, and
draw some comparisons between the flows here and those in gaseous giant planets.
Primary author
Matthew Browning
(University of Exeter)
