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About 10 per cent of intermediate- and high-mass dwarf stars are observed tohost a strong large-scale magnetic field at their surface, which is thought tobe of fossil field origin. However, there are few inferences as to the magneticfield strength and geometry within the deep interiors of stars. Consideringthat massive stars harbour a convective core whilst on the main sequence,asteroseismology of gravity (g) modes is able to provide constraints on theircore masses, yet it has so far not been used to probe the strength of theirinterior magnetic fields. Here we use asteroseismology to constrain an upperlimit for the magnetic field strength in the near-core region of the pulsatingand magnetic B star HD 43317, based on the expected interaction of a magneticfield and its g modes. We find a magnetic field strength of order $5 \times10^5$ G is sufficient to suppress high-radial order g modes and reproduce theobserved frequency spectrum of HD 43317, which contains only high-frequency gmodes. This result is the first inference of the magnetic field strength insidea main-sequence star.

Asteroseismic inference of the near-core magnetic field strength in the main sequence B star HD 43317