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Around 10% of white dwarfs exhibit global magnetic structures with fieldsranging from 1 kG to hundreds of MG. Recently, the first radiationmagnetohydrodynamics simulations of the atmosphere of white dwarfs showed thatconvection should be suppressed in their photospheres for magnetic fields withstrengths B $\gtrsim$ 50 kG. These predictions are in agreement with ourknowledge of stellar physics (e.g. energy transfer in strong magnetic fieldregions of the solar photosphere), but have yet to be directly confirmed fromwhite dwarf observations. We obtained COS far-UV spectroscopy of the weaklymagnetic, hydrogen-atmosphere, white dwarf WD2105-820 and of three additionalnon-magnetic, convective remnants (all in the $T_{\mathrm{eff}}$ range9000-11,000 K). We fitted both the COS and the already available opticalspectra with convective and radiative atmospheric models. As expected, we findthat for two of the non-magnetic comparison stars only convective model fitspredict consistent $T_{\mathrm{eff}}$ values from both the optical and the FUVspectra. In contrast, for WD2105-820 only the best fitting radiative modelproduced consistent results.

Can magnetic fields suppress convection in the atmosphere of cool white dwarfs? A case study on WD2105-820