The recent discovery of ubiquitous switchbacks, localized magnetic deflections in the nascent solar wind, by the Parker Solar Probe (PSP) has sparked interest in uncovering their origins. A prominent theory suggests these switchbacks originate in the lower corona through magnetic reconnection processes, closely linked to solar jet phenomena. Jets

Phase-correlation helioseismic holography of large sunspot in the 2.5--4.5-mHz p-mode spectrum, by Broock, Donea, Martinez & Lindsey show a signature that could be explained by fragmentation of magnetic flux into thin strands within the top few hundred km of sunspot subphotospheres. If so, this reinforces a hypothesis by Parker that such a

The Sun is depleted in refractory elements compared to nearby solar twins, which may be linked to the formation of giant or terrestrial planets. Here we present high-resolution, high signal-to-noise spectroscopic data for 17 solar-like stars hosting planets, obtained with Magellan II/MIKE, to investigate whether this depletion is related to planet

Context. The study of planetary nebulae (PNe) offers the opportunity to evaluate the efficiency of the dust production mechanism during the very late asymptotic giant branch (AGB) phases, which allows us to assess the role played by AGB stars as dust manufacturers. Aims. We studied the relationship between the properties of PNe, particularly the

Sub-Neptunes—volatile-rich exoplanets smaller than Neptune—are intrinsically the most common type of planet known. However, the formation and nature of these objects, as well as the distinctions between subclasses (if any), remain unclear. Two powerful tools to tease out the secrets of these worlds are measurements of (i) atmospheric composition

We use JWST/NIRISS slitless spectroscopy from the Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey to investigate the physical condition of 178 star-forming galaxies at 1.7 < z < 3.4. At these redshifts, the deep NGDEEP NIRISS slitless spectroscopy covers the [O II]λλ3726,3729, [O III]λλ4959,5007, Hβ and Hα emission features