Simulated stellar wind of TOI-1860, DS Tuc A, and HD 63433 in the x⋆ −y⋆ plane. The rotation axis lies along the positive z⋆. The Alfvén surface is shown as

Weighted mean abundance differences (large–small planet hosts) as a function of the chosen radius cutoff. Colored curves trace the various composite indices, with shaded bands showing uncertainties. The apparent volatile

Retrieved and training disk parameters for Earth-analogues. Left: single-planet per disk; Center: nominal, Right: two-planet systems. Training data is shown if both the planet mass and semi-major axis lies within

Simulated light curves for triple-lens systems where at least one planet lies in the resonant regime, as defined by the massratio-dependent boundaries (Equations 7) These configurations generally show strong central

Tricorders & Sensors Status Report Rapid Communications In Mass Spectrometry via PubMed December 27, 2025 Computer-aided design (CAD) model cross section of the MIP-MS prototype constructed for this study, including