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A super-massive Neptune-sized planet

Neptune-sized planets exhibit a wide range of compositions and densities, depending on factors related to their formation and evolution history, such as the distance from their host stars and atmospheric escape processes. They can vary from relatively low-density planets with thick hydrogen–helium atmospheres1,2 to higher-density planets with a substantial amount of water or a rocky interior with a thinner atmosphere, such as HD 95338 b (ref. 3), TOI-849 b (ref. 4) and TOI-2196 b (ref. 5). The discovery of exoplanets in the hot-Neptune desert6, a region close to the host stars with a deficit of Neptune-sized planets, provides insights into the formation and evolution of planetary systems, including the existence of this region itself. Here we show observations of the transiting planet TOI-1853 b, which has a radius of 3.46 ± 0.08 Earth radii and orbits a dwarf star every 1.24 days. This planet has a mass of 73 ....

United States , Collier Cameron , Telescopio Carlos , Monte Carlo , Exoplanet Community Early Release Science Program , Ames Research Center , Photometric All Sky Survey , Mission Conference , International Astronomical Union , Sloan Digital Sky , Plato Mission Conference , Kepler Science Operations Center , Meeting Of The American Astronomical Society , Program Working Group Tfop Wg Sub , Smithsonian Institution , Astrophysics Source Code Library , Gaia Early Data Release , Protoplanetary Cloud , Interest Catalog , Kepler Data Processing Handbook , Research Center , Observing Program Working Group , Sub Group , American Astronomical Society , Cumbres Observatory , Space Sci ,