On 10 May 2024, a powerful coronal mass ejection arrived at Earth at 17:05UT and caused a major geomagnetic storm. With the minimum SYM‐H excursion of −497 nT (5‐min data), this storm is the largest geomagnetic disturbance since March 1989, and can be categorized as a superstorm. In this work, by using ground‐based and space‐borne instruments, we focus on unusual aspects of the electrodynamic and ionospheric response to the May 2024 storm at middle and low latitudes.
The diffuse stellar component of galaxy clusters known as intracluster light (ICL) has been proposed as an observable tracer of the cluster’s dark matter (DM) halo. Assessing its reliability as a DM tracer requires understanding how the intracluster stars are energetically linked to the underlying DM distribution, which we investigate at $zapprox 0$ in 12 galaxy clusters with $M_{178} = 1.18 – 3.71 times 10^{14}, rm {M}_odot$ from the Horizon- AGN simulation.
This review explores the anomalous transport and acceleration of charged energetic particles in heliospheric and astrophysical plasmas. Traditional diffusion-advection models can be insufficient to fully describe the observed behavior of energetic particles, prompting the need for alternative frameworks based on non-Gaussian stochastic processes and fractional differential equations to capture regimes of subdiffusion and superdiffusion of energetic particles.
Earth observation data should inform decision making, but good decisions can only be made if the uncertainties in the data are taken into account. Making sense of uncertainty information can be difficult, because uncertainties represent the statistical spread in the observations (e.g., expressed as x±y), which does not relate directly to one specific use case of the data.
U‐shaped structures (or transient cusp‐shaped features) are special phenomena in ionograms, related to the electron density perturbations in the ionospheric F region. However, the mechanisms that trigger distinct shape structures, such as U‐shaped and hook‐shaped ones, are not fully understood yet.
This study statistically analyzes the electron precipitation patterns from 40 to 600 keV on dawnside and duskside and their correlations with geomagnetic activities and solar wind conditions based on Low‐Earth Orbit Fengyun‐3E (FY‐3E) satellite during July 2021 to May 2024. We found that for electrons less than 200 keV on dawnside between L shell of 6–10, the precipitation ratio (the ratio between precipitating flux and locally trapped flux) increases with increasing L and decreasing energy.
Mesoscale organization of boundary layer clouds modulates their radiative properties and contributes to the tropical hydrologic cycle. Trade wind cumuli (Cu) have varying organization and are a source of uncertainty in global climate models (GCMs). The linkage between Cu development and dynamics is difficult to capture, impacting low cloud feedback estimates.
Recent observations of the solar wind ions by the SPAN-I instruments on board the Parker Solar Probe (PSP) spacecraft at solar perihelia (Encounters) 4 and closer find ample evidence of complex anisotropic non-Maxwellian velocity distributions that consist of core, beam, and “hammerhead” (i.e., anisotropic beam) populations. The proton core populations are anisotropic, with T⊥/T∥ > 1, and the beams have super-Alfvénic speed relative to the core (we provide an example from Encounter 17).
Despite the well-established presence of amorphous compounds on planetary bodies such as the Moon and Mercury due to space weathering, the direct effect of atomic arrangement on the surface binding energies (SBEs) of elements on these bodies remains largely unexplored. Accurate SBE values are essential for reliably predicting sputtering yields and the energy distribution of ejecta.
Magnetic flux tubes in the presence of background rotational flows are abundant throughout the solar atmosphere and may act as conduits for MHD waves to transport energy throughout the solar atmosphere. Here we investigate the contribution from MHD waves to the Poynting flux in a 3D numerical simulation of a realistic solar atmosphere, modeling a structure resembling a solar vortex tube, using the PLUTO code in the presence of different plasma flow configurations.