Submitted by whawkins on September 10, 2014 - 9:25am
Sunspots are the most prominent manifestations of magnetic field in the visible layers of the solar atmosphere. Their origin is a dynamo process operating in the solar convection zone.
Overview and Research Goal
Submitted by kolinski on March 14, 2014 - 3:18pm
The Coronal Multichannel Polarimeter (CoMP) is being deployed this week!. To make room for this exciting new instrument, PICS had to be decommissioned (see our "PICS Removal Team" to the left) and CHIP had to be moved to another location on the spar. In PICS' place, a Coronado SolarMax60 telescope will be providing Halpha images. Look for upcoming changes to our homepage as these new instruments come online.
Submitted by kolinski on March 14, 2014 - 2:32pm
Submitted by kolinski on March 14, 2014 - 2:22pm
The FORWARD model is a suite of IDL and fortran codes that calculates simulated coronal polarization signals from numerical and analytical models of the corona. The images generated by the code are directly comparable to the CoMP data and can be used as guidelines to look for specific magnetic morphologies in the observational data. For more info see the FORWARD Model page.
The CoMP instrument (see Tomczyk, et al. 2008) can observe the coronal magnetic field with a full FOV in the low corona (~1.03 to 1.5 Rsun), as well as obtain information about the plasma density and motion. Like Solar-C, CoMP records the intensity and the linear and circular polarization (Stokes I,Q,U,V) of the forbidden lines of Fe XIII at 1074.7 nm and also at 1079.8 nm.
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