Phil Judge | High Altitude Observatory

Spectropolarimetric Insight into Plasma-Sheet Dynamics of a Solar Flare

Intensity and polarization data surrounding the current sheet formed on Sept 10 2017

Some thoughts on emission-line spectroscopy

Emission line data from IRIS are shown in the top panel. The lower panel lists an expression for the ratio of the emission lines shown of SI and O, under a minimal number of assumptions which often exceed the number of independent data points

Neutral hydrogen, helium and solar and stellar coronae

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

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

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

On single-point inversions of magnetic dipole lines in the corona

scattering geometry of point P is shown in the observer's frame with projections of the magnetic field components in this frame

Magnetic structure of the solar chromosphere-corona transition regions

Edge-enhanced images from near the core of the Mg II k line

Measuring the magnetic origins of solar flares, CMEs and Space Weather

A smoothed UV spectrum of α alpha Cen A, obtained by the Hubble Space Telescope

Atomic structure calculations of Land ́e g factors of astrophysical interest with direct applications for solar coronal magnetometry

Non-relativistic Land ́e g factor g(LS) for all LS terms (up to L = 10, S = 10) that couple into the total angular momentum J = 2Non-relativistic Land ́e g factor g(LS) for all LS terms (up to L = 10, S = 10) that couple into the total angular momentum J = 2. The grey area gathers all “forbidden” L and S values, i.e., if J > L+S or J < |L−S|.

The enduring mystery of the solar corona

Magnetic field lines in the corona

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