Research Highlights

Solar prominences are cool, dense condensations suspended in the million-degree corona by stressed magnetic fields. Because these fields store free magnetic energy before space-weather-relevant eruptions, prominence morphology provides a visible probe of otherwise hidden pre-eruptive coronal structure. A persistent observational puzzle is why filament barbs, the lateral extensions of prominences, show a preferred bearing linked to the chirality of the filament channel. Here we use a three-dimensional magnetohydrodynamic simulation of a condensation-formed prominence in an emerged flux rope to show that barb chirality arises from the coupling of helical magnetic geometry and magnetic Rayleigh--Taylor interchange.

Solar eruptions are powered by magnetic energy stored in the Sun’s atmosphere, but the magnetic structure that exists before an eruption is difficult to determine. In particular, scientists debate whether solar filaments are supported by pre-existing, twisted magnetic flux ropes or by less twisted magnetic arcades that form flux ropes only during eruption. We developed a physics-informed method that reconstructs the three-dimensional magnetic field using measurements from both the Sun’s visible surface and the chromosphere above it.

We present a data-inspired simulation of NOAA active region AR 11158. We simulate the formation of a collisional polarity inversion line (cPIL) by moving sunspots in a quadrupolar configuration along the centroid positions extracted from AR 11158. This process builds up free energy in the corona exceeding 4 × 10³² erg, out of which about 2 × 10³² erg are released in an X-flare followed by a series of smaller flares in the B to M range.

Coronal mass ejections (CMEs) are large eruptions of plasma from the Sun that can affect space weather near Earth. Coronagraphs observe these eruptions by measuring sunlight scattered by electrons in the solar corona and heliosphere. However, these images are two-dimensional projections of a three-dimensional structure, which makes it difficult to determine the true shape, density, and motion of a CME. We introduce SuNeRF-CME, a new method for reconstructing the three-dimensional plasma structure of CMEs from coronagraph images taken from multiple viewpoints.

Solar physicists use instruments called polarimeters to measure the polarization of sunlight, which reveals the strength and structure of the Sun's magnetic field. Before a polarimeter can deliver reliable measurements, it must be calibrated by feeding known polarization states into the instrument. Calibration takes time, and telescope time is precious — particularly for solar telescopes, where intense sunlight limits how long calibration optics can safely remain in the beam. This raises a key question: what sequence of calibration measurements yields the most accurate result in a given amount of time?

The large-scale traveling ionospheric disturbances (LSTIDs) over the Asian-Pacific sector during the 10-11 May 2024 superstorm are investigated using ionosonde observation and simulation from a whole geospace model - Multiscale Atmosphere Geospace Environment (MAGE), which fully couples multiple magnetosphere, ionosphere and thermosphere models.

A balloon-borne instrument called HIWIND was launched from New Zealand to observe thermospheric winds in the mid-latitudes. The observed winds were compared with TIEGCM model simulation and were found to be much larger than the simulated results.

We address the need to model the effects of radiation anisotropy and atomic coherence on the Stokes profiles
of magnetically-sensitive lines formed in the solar chromosphere. Accounting for the physics of scattering polarization associated with these effects, and how they map to the strength and direction of weak magnetic fields on the Sun is a formidable computational task when done fully self-consistently. This has hindered the broad heliophysics community from gaining prompt access to reliable data products from solar facility spectro-polarimeters concerning quiet-Sun magnetism.

Authors R. Casini, D. Harrington, and A. de Wijn review the algebraic definition of the efficiency of a polarization modulation scheme, which is commonly adopted for solar and stellar spectro-polarimetry applications, and generalize it to allow distinct states of the modulation cycle to have arbitrary throughput and different photon-noise statistics for each state.