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Derivation of Instrument Requirements for Polarimetry using Mg, Fe, and Mn lines between 250 and 290 nm

IRIS map

Watch the BBC's Interview with Philip Judge—The Sun: Myths and Magnetism

The Sun: Myths and Magnetism

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

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

Optimal spectral lines for measuring chromospheric magnetic fields

The solar spectrum seen at low resolution, below the atmospheric cutoff at 3100 Angstrom

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

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.

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

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

The 2017 Total Eclipse was a Life-changing Four Minutes

Jenna Samra, taken on the Gulfstream V research aircraft

P Judge and R Casini Advise Early Career Researchers

Phil Judge and Roberto Cassini

AAS Nova Features a Recent Publication by Philip Judge

Images to highlight the corrugated surfaces at which the centers of UV lines are formed (close to τ = 1) in MURaM calculations of the upper solar chromosphere

Sun-Like Stars Shed Light on Solar Climate Forcing

Seasonally averaged data for the CaII“S-index” and for the average magnitudes of the Strömgrenbplusy filters are shown for the star 18 Sco

Pagination

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This material is based upon work supported by the NSF National Center for Atmospheric Research, a major facility sponsored by the U.S. National Science Foundation and managed by the University Corporation for Atmospheric Research. Any opinions, findings and conclusions or recommendations expressed in this material do not necessarily reflect the views of the U.S. National Science Foundation.