3D Coronal Magnetic Field Reconstruction Based on Infrared Polarimetric Observations

Monday, 15 December 2014
Haosheng Lin, Institute for Astronomy, Honolulu, HI, United States, Maxim Kramar, Catholic University of America, Washington, DC, United States and Steven Tomczyk, National Center for Atmospheric Research, Boulder, CO, United States
Measurement of the coronal magnetic field is a crucial ingredient in understanding the nature of solar coronal phenomena at all scales. A significant progress has been recently achieved here with deployment of the Coronal Multichannel Polarimeter (CoMP) of the High Altitude Observatory (HAO). The instrument provides polarization measurements of Fe xiii 10747 A forbidden line emission. The observed polarization are the result of a line-of-sight (LOS) integration through a nonuniform temperature, density and magnetic field distribution. In order resolve the LOS problem and utilize this type of data, the vector tomography method has been developed for 3D reconstruction of the coronal magnetic field. The 3D electron density and temperature, needed as additional input, have been reconstructed by tomography method based on STEREO/EUVI data. We will present the 3D coronal magnetic field and associated 3D curl B, density, and temperature resulted from these inversions.