We use rotation splittings derived from very long and long time series, namely 25.2, 12.6, and 6.3 yr long, computed by S. G. Korzennik independent methodology to characterize the solar tachocline and its variation with latitude and time. We use two different inversion methodologies and a model of the tachocline to derive its position, its width

The magnetic fields in the solar polar region are important to our understanding of the internal dynamo process, the global coronal structure, and the origin of the solar wind. The inference of polar fields based on spectropolarimetric observation is highly model-dependent and can suffer from various systematic effects. Here, we analyze a raster

We investigate the feasibility of detecting decameter-scale objects on day-side trajectories in infrared wavelengths from space, prior to their close encounters with Earth. Specifically, we examine a 20-m object on a Chelyabinsk-progenitor orbit (Jan/Feb 2013) and the 60-m potentially hazardous asteroid 2024 YR4 (Nov/Dec 2024 & 2032) during their

Context. The flat spectrum radio quasar (FSRQ) OP 313 was discovered in December 2023 in very-high-energy γ rays above 100 GeV, enabling for the first time a complete broadband characterization of its emission. However, the lack of updated measurements of its accretion disc, broad line region, and dusty torus hampers a detailed interpretation of

Small-scale jet-like eruptions, such as picoflare jets and jetlets, are recognized as potential contributors to coronal heating and solar wind acceleration, yet their physical origin is still not fully established. Using ultra-high-resolution extreme ultraviolet imaging datasets from the Extreme Ultraviolet Imager on board the Solar Orbiter mission

The ∼200,000 stars observed by the Kepler mission have provided unprecedented constraints across astrophysics. With the advent of modern spectroscopic and photometric surveys, new limits in stellar characterizations are within reach. In this work, we report a compilation of atmospheric parameters (T eff, log ( g ) , and [M/H]) for the Kepler stars