solar magnetism | High Altitude Observatory

Erratum: Analysis of Seeing-Induced Polarization Cross-Talk and Modulation Scheme Performance

Graph of polarimetric errors

New Book! The Problem of Coronal Heating: A Rosetta Stone for Electrodynamic Coupling in Cosmic Plasmas

Cover of Phil Judge's book, The Problem of Coronal Heating

MLSO UCoMP Science Data Now Available

UCoMP data on MLSO website.

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

IRIS map

Designing a New Coronal Magnetic Field Energy Diagnostic

Non-potentiality diagnostics of the energized flux-rope simulation at time step 89

Solar Transition Region UltraViolet Explorer (STRUVE) requirements flow down to design

Flow chart showing requirements from 3 science questions

On the (Mis)interpretation of the Scattering Polarization Signatures In the Ca II 8542 A line Through Spectral Line Inversions

Inversion results for observing geometries away from the disk center

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.

The Coronal Veil

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.

Subscribe to solar magnetism