The K-Cor coronagraph has been specifically designed to study the formation and dynamics of coronal mass ejections and the evolution of the density structure of the low corona.

The CoMP instrument 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.

The Precision Solar Photometric Telescope (PSPT) is the centerpiece of the National Science Foundation (NSF) Radiative Inputs from Sun to Earth (RISE) program whose aim is to measure and understand variability in the solar radiative output.

CHIP is a differential device using properties of the Helium-I line at 1083 nm as an indicator of both chromospheric and coronal structures.

PICS took images of the solar disk and limb in H-alpha (656.3nm) from 1997 until 2010, when it was decommissioned. A Coronado SolarMax telescope provided H-alpha from 2010-2011. Currently, our H-alpha images are provided by the GONG Network.

The Mark-III instrument was the third generation white light K-coronameter instrument at MLSO, and it operated from 4 February, 1980 through 1999. Mk4 built upon this success and operated from 1999 well into 2013.

The Coronagraph/Polarimeter (C/P) aboard the SMM satellite was provided by HAO to study the relationship of the corona to the flare process. The C/P used an arrangement of multiple internal and external occulting discs to block out the direct light from the Sun's photosphere, thereby permitting the faint light of the Sun's outer corona to be recorded.

The MK I K-coronameter was the first instrument to observe the white light corona outside of a total solar eclipse. It recorded scans of the polarization brightness (pB) of the Thomson scattered K-Corona continuum emission at three heights between 1.12 and 2 solar radii.