The Mauna Loa Solar Observatory (MLSO) occupies part of the NOAA Mauna Loa research site located on the flank of Mauna Loa at an elevation of 3440 meters on the island of Hawaii. It is operated by the High Altitude Observatory, a division of the National Center for Atmospheric Research, which is located in Boulder, Colorado.
Mission Lifetime: 1956 to 1978
The slides in this collection were written By P. Charbonneau and O.R. White–April 18, 1995.
Submitted by kolinski on November 16, 2016 - 10:41am
Determining the state of the corona prior to coronal mass ejections (CMEs) is crucial to understanding and ultimately predicting solar eruptions. A common and compelling feature of CMEs is their three-part morphology as seen in white light observations of a bright expanding loop, followed by a relatively dark cavity, and lastly a bright core associated with an erupting prominence/filament.
Here is a catalogue providing detailed analysis of 98 white light cavities observed by MLSO's Mk4 coronameter:
Submitted by whawkins on August 3, 2016 - 4:06pm
Lisa is a Visiting Scientist here at HAO since September 2014 and also is currently working for Space Systems Research Corporation. In the spring of 2017, Lisa will begin a NSF postdoctoral fellowship at HAO, working as a collaborator with the dynamo group.
Submitted by whawkins on July 25, 2016 - 3:47pm
Giuliana de Toma is a Project Scientist in the High Altitude Observatory of NCAR specializing in solar cycle variability and its influence on the corona and heliosphere.
Submitted by whawkins on April 14, 2016 - 10:54am
Dr. Steven Tomczyk is a Senior Scientist and Section Head in the High Altitude Observatory at the National Center for Atmospheric Research. He has spent his career developing instrumentation for the remote sensing of magnetic and velocity fields on the Sun.
Submitted by whawkins on April 14, 2016 - 9:55am
Dr. Scott McIntosh is Observatory Director in the High Altitude Observatory at the National Center for Atmospheric Research. His primary focus of research is chromospheric dynamics and understanding the physical connectivity between the Sun's cool surface and its considerably hotter corona.
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