Abstract
Spectropolarimetic campaigns have established that large-scale magnetic fields are present at the surfaces of approximately 10% of massive dwarf stars. However, there is a dearth of magnetic field measurements for their deep interiors. Asteroseismology of gravity-mode pulsations combined with rotating magneto-hydrodynamical calculations of the early-B main-sequence star HD 43317 constrain its magnetic field strength to be approximately 5 × 105 G just outside its convective core. This proof-of-concept study for magneto-asteroseismology opens a new window into the observational characterisation of magnetic fields inside massive stars.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 218-223 |
| Number of pages | 6 |
| Journal | Proceedings of the International Astronomical Union |
| Volume | 18 |
| DOIs | |
| State | Published - May 1 2022 |
Funding
DMB and TVR gratefully acknowledge funding from the Research Foundation Flanders (FWO) by means of senior and junior postdoctoral fellowships with grant agreements 1286521N and 12ZB620N, respectively, and FWO long stay travel grants V411621N and V414021N, respectively. DL is supported in part by the US National Aeronautics and Space Administration (NASA) grant 80NSSC20K1280. Computations were conducted with support by the NASA High End Computing Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center on Pleiades with allocation GIDs s2276. This research was supported in part by the National Science Foundation under grant no. NSF PHY-1748958.
Keywords
- magnetic fields
- stars: early-type
- stars: oscillations
- stars: rotation
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science