Astrobiology42- Page

Stability analysis of the TOI-6041 system. The phase space of the system is explored by varying the orbital period Pi and eccentricity ei of each planet independently. For each initial

Representation of metadata factors grouped as environmental factors, operational constraints, experimental design, and assay type for dataset GLDS-37. We exclude the metadata categories that were not populated for this dataset.

Homöller plots of the time- and horizontal-mean vertical profiles of equivalent potential temperature (colors) in each constant-𝛽 simulation. Values from within the model sponge layer are not shown. The black

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

Planet Venus: Japan’s Venus Climate Orbiter Ultraviolet View December 23, 2016 – JAXA Context: Planets in the HZ can have dense atmospheres affecting their rotations. Over time, the rotation tends