The energy budget of stellar magnetic fields : comparing non-potential simulations and observations
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The magnetic geometry of the surface magnetic fields of more than 55 cool stars have now been mapped using spectropolarimetry. In order to better understand these observations, we compare the magnetic fieldt opology at different surface scale sizes of observed and simulated cool stars. For ease of comparison between the high-resolution non-potential magnetofrictional simulations and the relatively low-resolution observations, we filter out the small-scale field in the simulations using a spherical harmonics decomposition. We show that the large-scalefield topologies of the solar-based simulations produce values of poloidal/toroidal fields and fractions of energy in axisymmetric modes that are similar to the observations. These global non-potential evolution model simulations capture key magnetic features of the observed solar-like stars through the processes of surface flux transport and magnetic flux emergence. They do not, however, reproduce the magnetic field of M-dwarfs or stars with dominantly toroidal field.Furthermore, we analyse the magnetic field topologies of individual spherical harmonics for the simulations and discover that the dipole is predominately poloidal, while the quadrupole shows the highest fraction of toroidal fields. Magnetic field structures smaller than a quadrupole display a fixed ratio between the poloidal and toroidal magnetic energies.
Lehmann , L T , Jardine , M M , Vidotto , A A , Mackay , D H , See , V , Donati , J-F , Folsom , C P , Jeffers , S V , Marsden , S C , Morin , J & Petit , P 2016 , ' The energy budget of stellar magnetic fields : comparing non-potential simulations and observations ' Monthly Notices of the Royal Astronomical Society: Letters , vol Advance Access . DOI: 10.1093/mnrasl/slw225
Monthly Notices of the Royal Astronomical Society: Letters
© 2016, the Author(s). This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at mnrasl.oxfordjournals.org / https://doi.org/10.1093/mnrasl/slw225
LTL acknowledges support from the Scottish Universities Physics Alliance (SUPA) prize studentship and the University of St Andrews Higgs studentship. MMJ and VS acknowledge a Science & Technology Facilities Council (STFC) postdoctoral fellowship.
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