Dynamics of Solar Flare Loops: Spectral Diagnostics

Solar flares are one of the most energetic events in the solar atmosphere. The eruption of a solar flare releases energy and leads to plasma heating, particle acceleration, waves, mass flows, etc.. Mass motions are dynamic response to the flare heating and also plasma cooling in different evolution stages, represented by evaporation and condensation in the chromosphere and also plasma draining in the corona. In this project we will study these mass motions and their evolution throughout a solar flare.

Dynamic mass motions can be detected through Doppler shift measurements in spectral lines formed in different atmospheric layers. The recently launched Interface Region Imaging Spectrograph (IRIS) is providing high-resolution spectroscopic (and also slit-jaw imaging) data in the UV wavelength range that focus on chromosphere and transition region (i.e., the interface region between photosphere and corona). In addition, EUV spectroscopic data focusing on the hot corona are observed by the EUV Imaging Spectrometer (EIS) onboard Hinode satellite. By analyzing the UV and EUV spectroscopic data, we can diagnose mass motions from the chromosphere and transition region to the corona.

In this project, student will learn how to analyze the spectroscopic data from IRIS and EIS, as well as imaging data from Solar Dynamics Observatory (SDO). We will learn about dynamic mass motions in different flaring atmospheric layers during the flare and understand the dynamic response to flare heating and plasma cooling. Experience with IDL or similar programming languages is desired though not required.