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September 27, 2016

If you have visited the High Altitude Observatory, you may recall seeing the Maunder’s original butterfly diagram. The chart resembles three butterflies traveling west. Drawn by Annie S.D. Maunder and E. Walter Maunder, it demonstrated for the first time the movement of sunspot emergence from the poles toward the equator over the sun's 11-year cycle.

Azaymi Litzi Siu Tapia
September 22, 2016

Azaymi Litzi Siu Tapia is currently a PhD student in Solar Physics at Max Planck Institute for Solar System Research and the University of Gottingen in Germany, since August 2014. She is working with Andreas Lagg and Sami K. Solanki on the physical mechanisms responsible for driving photospheric flows in the penumbra of sunspots.

September 6, 2016

Kevin Dalmasse is currently finishing a 2-year postdoc jointly funded by CISL and an Air Force grant from HAO Senior Scientist, Sarah Gibson. His current postdoc is on data constrained reconstruction of the solar coronal magnetic field, with the goal of better constraining/quantifying the 3D properties of eruptive solar magnetic fields (for Space Weather predictions).

Publication Highlights

Polar view of absolute GPS TEC difference
September 28, 2016

There are still uncertainties regarding the formation mechanisms for storm-enhanced density (SED) in the high and subauroral latitude ionosphere.

SDO/AIA 171Å sub-fields
September 14, 2016

The Interface Region Imaging Spectrograph (IRIS) provides an unparalleled opportunity to explore the (thermal) interface between the chromosphere, transition region, and the coronal plasma observed by the Atmospheric Imaging Assembly (AIA) of the Solar Dynamics Observatory (SDO).

Poloidal and toroidal magnetic fields
September 8, 2016

We implement an Ensemble Kalman Filter procedure using the Data Assimilation Research Testbed for assimilating "synthetic" meridional flow-speed data in a Babcock–Leighton-type flux-transport solar dynamo model.

MLSO Latest Images

H-alpha Disk and Limb

Currently, H-alpha images are obtained by the GONG network, operated by the National Solar Observatory .


CoMP Coronal Intensity

The COronal Multi-channel Polarimeter (CoMP) observes the Fe-XIII emission line at 1074.7 nm to measure the coronal magnetic field and obtain plasma density and motion in the low corona from ~1.03 to 1.5 solar radii.


K-Cor White Light Corona

Designed to study the formation and dynamics of coronal mass ejections and the evolution of the density structure of the low corona, K-Cor records the polarization brightness (pB).


K-Cor (radially graded filter)

K-Cor image with filter applied to maximize image contrast, especially in the outer field.

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