Title: Jets in the Solar Atmosphere |
Type of Project: Data Analysis
Interest in analyzing space-based observations.
Some programming skills required. The data analysis will be performed
primarily using IDL.
Mentor: Dr. Mari Paz Miralles and Dr. John Raymond
Email: mmiralles_at_cfa.harvard.edu and jraymond_at_cfa.harvard.edu
Magnetic reconnection is one of the most important processes in the
solar corona. Reconnection occurs when the magnetic field lines of a
highly conducting plasma are broken and rejoined, thus changing the
magnetic connectivity of the system. This process is responsible for
mass and energy release during solar jets. Observations show solar
jets traveling at large altitudes in the solar corona without falling
back into the lower atmosphere .
The goal of this project will be to characterize the jet plasma and
dynamics as the jets propagate in the open field regions of the solar
wind. To accomplish this goal, we will determine their kinematic
properties and trace the jet response into the inner heliosphere. For
these tasks we will analyze recent solar jet event images from Hinode/XRT,
SDO/AIA, STEREO/SECCHI, and SOHO/LASCO.
Figure: Hinode/XRT observations of a standard coronal jet in the
northern polar coronal hole (from ).
 Miralles, M. P. et al. 2012, ApJ, in preparation
 Moore et al. 2010, ApJ, 720, 757