![[LEFT] GJ 536 b and c in context. The upper panel shows the masses of known planets, for masses below 100 M⊕, and periods shorter than 1000 days, with the planets of the system of GJ 536 highlighted, and the solar system planets as reference. The middle panel shows the same, but as a function of insolation. The lower panel shows the contrast in reflected light of low-mass planets orbiting bright stars (mV < 12), compared to their angular separation to their parent star. The dotted vertical lines indicate the limits in which ANDES wil be able to observe (Palle et al. 2025). The red symbols for the planets of GJ 536 show the potential range of contrasts. The green squares show the position of the ANDES golden sample. [RIGHT] Parameters of the planets of the system of GJ 536, using the adopted (circular) model. -- astro-ph.EP](https://i0.wp.com/astrobiology.com/wp-content/uploads/2025/09/A-Second-Lowmass-Planet.png?resize=1200%2C719&ssl=1)
GJ 536 is a low-mass star, located 10 pc away from the Sun, that hosts a low-mass planet orbiting with a period of 8.71 days.
Doppler Imaging
Posted inAstronomy & Telescopes, Exoplanets, -moons, -comets, Imaging & Spectroscopy, Space Weather & Heliophysics, Status Report, Stellar Cartography
Using Doppler Imaging To Model Stellar Activity And Search For Planets Around Sun-like Stars
Doppler Imaging (DI) is a well-established technique to map a physical field at a stellar surface from a time series of high-resolution spectra.