LHS 475

LHS 475 is a red dwarf star located approximately 41 light-years away in the constellation Octans. It is significantly smaller and cooler than our Sun, which is characteristic of M-dwarf stars. This type of star is among the most common in the Milky Way galaxy.

The LHS 475 system gained prominence due to the discovery of an exoplanet, LHS 475 b, orbiting it. LHS 475 b was detected using transit photometry data from NASA's Transiting Exoplanet Survey Satellite (TESS). Confirmation of the planet's existence and characteristics was subsequently achieved through observations with the James Webb Space Telescope (JWST).

LHS 475 b is a rocky, Earth-sized exoplanet. It orbits its host star very closely, resulting in a short orbital period of approximately two days. Due to its proximity to LHS 475, the planet is likely tidally locked, meaning one side permanently faces the star, while the other is in perpetual darkness.

Initial observations with JWST suggested the potential absence of a thick atmosphere on LHS 475 b. However, further analysis and observations are needed to definitively characterize the planet's atmospheric properties and habitability potential. Red dwarf stars, while long-lived, are known for their high levels of stellar activity, including flares, which could potentially impact the atmospheres of orbiting planets.