Inferring micro-turbulent magnetic fields via the Hanle effect
Abstract
A key research problem in solar physics is to understand the small-scale magnetic fields that permeate the solar surface. These fields are too weak to be observed through conventional methods (e.g. Zeeman splitting in a spectral line). However, the high spatial and spectral resolution of DKIST will facilitate novel ways of probing the magnetic field. One such method relies on the Hanle effect.
When an atmosphere is illuminated anisotropically, the emerging radiation will be polarized. Furthermore, if a magnetic field is present, the observed polarization is reduced due to the Hanle effect. We aim to show that the Hanle effect can be used to map out the structure of microturbulent magnetic fields - potentially providing new insights into MHD turbulence in the quiet Sun.- Publication:
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Solar Heliospheric and INterplanetary Environment (SHINE 2019)
- Pub Date:
- May 2019
- Bibcode:
- 2019shin.confE.172K