Context. Solar Orbiter and the Daniel K. Inouye Solar Telescope (DKIST) are two of the newest facilities available to the solar physics community. The first coordinated observations of the Sun by these two facilities occurred over the course of one week in October 2022. The returned data are open-access and will provide a valuable resource to researchers in the field. Aims.
The nature of the elusive dark matter can be probed by comparing the predictions of the cold dark matter framework with the gravitational field of massive galaxy clusters. However, a robust test of dark matter can only be achieved if the systematic uncertainties in the reconstruction of the gravitational potential are minimized.
Orbital remote sensing has shown that some regions of the ancient Martian crust contain hundreds of discrete terrains covered by chloride‐rich evaporites. In terrestrial evaporitic systems, evaporite sequences typically begin with the deposition of carbonates, followed by sulfates, and finally chlorides, a depositional sequence that has not yet been found on Mars.
The recent alignment of CryoSat-2 to maximise orbital coincidence with the Ice, Cloud, and land Elevation Satellite-2 (ICESat-2) over the Southern Ocean and Antarctica in July 2022, known as the CryoSat-2 and ICESat-2 (CRYO2ICE) Resonance Campaign, provided an opportunity to validate these satellites over land and sea ice.
We investigate numerically the energy flow and radiation efficiency of accreting neutron stars as potential ultraluminous X-ray sources (ULXs). We perform 10 simulations in radiative general relativistic magnetohydrodynamics, exploring six different magnetic dipole strengths ranging from 10 to 100 GigaGauss, along with three accretion rates, 100, 300, and 1000 Eddington luminosity units.
We analyze ozone trends in the upper troposphere and lower stratosphere (UTLS, ∼ ${sim} $300–50 hPa), using geographical (latitude‐pressure and latitude‐altitude) and, for the first time, dynamical (equivalent latitude‐potential temperature, EqL‐θ $theta $) coordinates. Trends are determined using linear least squares fits, multiple linear regression, and dynamical linear modeling.
Context. In solar-like oscillators, acoustic waves are excited by turbulent motion in the convective envelope and propagate inward, generating a variety of standing pressure modes (p modes). When combining the power of several solar acoustic modes, some studies have reported an excess that is not compatible with pure stochastic excitation. This excess could be a signature of a second mode excitation source. Aims.
We report on prolonged enhancements of electron fluxes at energies at or above 500 keV, observed in the magnetotail by the lunar‐orbiting Acceleration, Reconnection, Turbulence, and Electrodynamics of Moon’s Interaction with the Sun (ARTEMIS) during the recovery phase of a magnetic storm with minimum Dst ${D}_{st}$ ≈ ${approx} $ −200 nT during periodic auroral electrojet (AE $AE$) activations.
Despite the fact that the terrestrial planets all formed from the protoplanetary disk, their bulk compositions show marked departures from that of material condensing from a canonical H2-rich solar nebula. Metallic cores fix the oxygen fugacities (fO2s) of the planets to between ∼5 (Mercury) and ∼1 log units below the iron-wüstite (IW) buffer, orders of magnitude higher than that of the nebular gas.