The Sun’s magnetic field undoubtedly plays a central role in many solar phenomena. For example, the topology of the magnetic field appears to be a critical element in determining if an active region will give rise to a coronal mass ejection. Understanding the properties of solar magnetic fields is also important to determining the physical mechanisms that produce the high temperature plasma observed in both the quiescent corona and in solar flares. This program explores the link between solar magnetic fields and the structure and dynamics of the corona using a combination of high spatial, spectral, and temporal resolution solar observations and numerical models. This research makes extensive use of observations from instruments on the Hinode, SDO, and STEREO missions.

 

key words

Solar physics; Solar atmosphere; Solar magnetic fields; Solar flares; Ultraviolet astronomy; X-ray astronomy; Numerical models and analyses;

Citizenship:  Open to U.S. citizens and permanent residents

Level:  Open to Postdoctoral applicants