Coronal Solar Magnetism

Magnetic Nulls and Super-radial Expansion in the Solar Corona

Coronal pseudostreamer magnetic topology
Monday, May 1, 2017

Magnetic fields in the sun's outer atmosphere, the corona, control both solar-wind acceleration and the dynamics of solar eruptions.

DKIST: Solar Physics in Service of Society

Phil Judge, Claire Raftery, Sarah Jaeggli

Philip Judge, Senior Scientist at HAO, Claire Raftery, Director of Education and Outreach at NSO HQ in Boulder, and Sarah Jaeggli, Assistant Astronomer at the NSO's Daniel K Inouye Solar Observatory in Maui were guests on KGNU public radio in Boulder, CO.

Sunspots and Photospheric Dynamics

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.

Solar Transients and Space Weather

Overview and Research Goal

CoMP is being deployed

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.

CoMP Data Now Available

Coronal Multichannel Polarimeter (CoMP) data are now available from the MLSO data calendar. Expect the number of days with processed data to increase in the coming weeks, so check back often!

The FORWARD Model

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.

COronal Multi-channel Polarimeter

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.

MLSO Data and Movies

Pages

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