Two rows of colorful squares, 8 total, showing coronal geyser jet action
Sep 21, 2022

Thermal and Non-thermal Properties of Active Region Recurrent Coronal Jets Publication Name

Coronal hole centroid latitude vs. Carrington Rotation
Aug 31, 2022

Study of Coronal Hole Lifetimes

CLEDB 2-line magnetic inversion algorithm flowchart. An important aspect is the delivery of multiple possible solutions for each observation at the last step. Note that the x-coordinate of the point in space, as well as nearest electron density, are returned along with B. The figure uses the notation Vobs and Vdb for observed and computed values of the amplitudes of the Stokes parameters corresponding to O3 and S3 (B = 1) in the text.
Jul 11, 2022

Efficient and Automated Inversions of Magnetically-Sensitive Forbidden Coronal Lines: CLEDB - The Coronal Line Emission DataBase Magnetic Field Inversion Algorithm

3D view of the simulated corona; bottom panel: magnetogram; back panel: synthetic AIA 211A coronal image; middle vertical plane: volumetric emissivity. Field lines are included for reference.
Jul 11, 2022

The Coronal Veil

Fe XIII 1074.68 nm emission over atmospheric absorption (normalized) in the He I Cryo-NIRSP wavelength range with all labeled candidate lines.
Jul 11, 2022

A Spectroscopic Survey of Infrared 1–4 μm Spectra in Regions of Prominent Solar Coronal Emission Lines of Fe XIII, Si X, and Si IX

Electrical engineer, Brandon Larson, and Technician Rob Graves install the K-cor center section onto the solar spar at the NCAR Mesa Lab in Boulder
Dec 1, 2021

A New Coronagraph for Mauna Loa

Average temperature of 35 cavities (black) and their surrounding streamers (red)
Nov 18, 2021

Thermal Properties of Coronal Cavities

Fully processed image of the corona generated by stacking many co-aligned, calibrated images and applying a radial filter and multi-scale unsharp mask to bring out details at higher altitudes
Nov 18, 2021

A new facility for airborne solar astronomy: NASA’s WB-57 at the 2017 total solar eclipse

Line profiles of He I and He II resonance lines are shown as a function of wavelength (and equivalent Doppler shift) and time, computed from a coronal initial state
Nov 17, 2021

Neutral hydrogen, helium and solar and stellar coronae

A comparison of 1D and 3D calculations of the brightness of Ca II K (top row), Mg II k (middle row) and H Lα (bottome row), computed as for the k line images, at the Doppler shifts shown
Nov 17, 2021

On the Cores of Resonance Lines Formed in the Sun's Chromosphere

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