Stellar rotation is closely linked to both the age and the magnetic activity of stars. Through gyrochronology, studying stellar rotation provides a means to estimate stellar ages and trace the evolution of planetary systems, and it is also a crucial means to constrain and correct stellar activity effects for robust exoplanet detection and

Tracing the compositional link between terrestrial super-Earths and their host stars provides clues about their dominant formation pathway. By constraining the stellar abundances of refractory elements, we can predict the core mass fractions (CMFs) of their super-Earths. The level of agreement between this prediction and the planetary CMF derived

We present a far-ultraviolet (FUV) analysis of the star-forming complexes (SFCs) in the nearby spiral galaxy NGC 2090 based on observations from the Ultraviolet Imaging Telescope, and compare the FUV emission with that from the optical and infrared bands. NGC 2090 exhibits prominent star formation in its extended outer disk, with FUV emission

Context. Finding low-mass planets around solar-type stars requires understanding the physical variability of the host star, which greatly exceeds the planet-induced radial-velocity modulation. Different solar photospheric absorption lines have slightly disparate responses to stellar activity, which should permit us to disentangle the wavelength

Pre-explosion mass loss in supernova (SN) progenitors is a crucial unknown factor in stellar evolution, yet has been illuminated recently by the diverse zoo of interacting transients. We present SN 2024cld, a transitional core-collapse SN at a distance of 39 Mpc, straddling the boundary between SN II and SN IIn, showing persistent interaction with

We report a rotational light curve and Fourier baseline model for the Jupiter Trojan (15094) Polymele, a primary target of the NASA Lucy mission, obtained on 2026 May 19─20 and May 21─22 UT with the Two-meter Twin Telescope (TTT). Phase-Dispersion Minimization over the combined two-night dataset yields P rot = 5.762 ± 0.051 hr and a peak-to-peak