TOI-1203 d Archives - Astrobiology

Stability analysis of the TOI-1203 system in the orbital period-eccentricity domain: planet b (top left), c (top right), d (bottom left), and e (bottom right). For fixed initial conditions, the phase space of the system is explored by varying the orbital period Pi and eccentricity ei of each planet independently. For each initial condition, the system is integrated over 40 kyr, and a stability criterion is derived with the frequency analysis of the mean longitude. The chaotic diffusion is measured by the variation in the frequencies and the color scale corresponds to the decimal logarithm of the stability index D. The red zone corresponds to highly unstable orbits, while the dark blue region can be assumed to be stable on a billion-year timescale. The current positions of the planets are marked with circles in each plot, and error bars represent the observational uncertainties (Tables B.2 and B.3). The white dashed vertical lines correspond to the main MMRs in the system. -- astro-ph.EP

Astronomy & Telescopes, Exoplanets, -moons, -comets, Imaging & Spectroscopy, Press Release

A Four-planet System Orbiting The Old Thick Disk Star TOI-1203

by Keith CowingSeptember 17, 2025September 17, 2025

TOI-1203 is a bright (V=8.6) G3 V star known to host a transiting warm sub-Neptune on a 25.5 d orbit.