corona | High Altitude Observatory

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

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

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

Mapping the magnetic field in the solar corona through magnetoseismology

Analysis results for the observation on November 3, 2016 (dataset D2)

Reconstructing the Coronal Magnetic Field: The Role of Cross-Field Currents in Solution Uniqueness

Comparison of analytic model magnetic field lines to results of numerical reconstruction

Simulations of prominence eruption preceded with large amplitude longitudinal oscillations and draining

An MHD simulation of the evolution of a prominence-forming twisted coronal flux rope, for which large amplitude longitudinal (LAL) oscillations are excited during the quasi-static rise phase, followed by prominence draining towards the flux rope foot-points and the eventual eruption of the flux rope and the prominence

Detecting the Chromospheric Footpoints of the Solar Wind

SDO and IRIS full-disk observations from 2016 Feb 22

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

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|.

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