description LHS 1140 b Overview
LHS 1140 b is an exoplanet approximately seven times Earth’s mass, orbiting the M-dwarf star LHS 1140. Its location within the habitable zone—the region around a star where liquid water could exist on a planet's surface—makes it significant for astronomical research. Scientists study this super-Earth to understand planetary atmospheres and assess its potential habitability. The system is of particular interest to researchers investigating planets orbiting red dwarf stars.
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What type of planet is LHS 1140 b?
LHS 1140 b is categorized as a super-Earth, meaning it is a rocky planet larger than Earth but smaller than Neptune. It has a radius about 1.4 times that of Earth. It is significantly denser than our planet, suggesting a large iron core.
When was LHS 1140 b discovered?
The exoplanet was discovered in 2017 by the HARPS (High Accuracy Radial velocity Planet Searcher) instrument in Chile. The discovery was soon confirmed by NASA's Spitzer Space Telescope. It orbits a red dwarf star roughly 40 light-years away in the constellation Cetus.
Why is LHS 1140 b a good target for atmospheric study?
LHS 1140 b is located within the habitable zone of its host star, where liquid water could theoretically exist. Additionally, it transits its star frequently and its star is relatively quiet, making it highly favorable for atmospheric characterization. NASA's James Webb Space Telescope has flagged it as a prime target.
Does LHS 1140 b orbit a Sun-like star?
No, it orbits a red dwarf star, which is much cooler and smaller than our Sun. Because the star is cooler, the planet's close orbit still places it in the habitable zone. Red dwarfs are the most common type of star in the Milky Way galaxy.
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