The UV environment of a host star affects the photochemistry in the atmosphere, and ultimately the surface UV environment for terrestrial planets and therefore the conditions for the origin and evolution of life.
The prospect of finding ocean-bearing exoplanets has been boosted, thanks to a pioneering new study. An international team of scientists, including from the University of Exeter, has discovered an immense cloud of hydrogen escaping from a Neptune-sized exoplanet.
We model the atmospheres and spectra of Earth-like planets orbiting the entire grid of M dwarfs for active and inactive stellar models with Teff = 2300K to Teff = 3800K and for six observed MUSCLES M dwarfs with UV radiation data.
Understanding whether M-dwarf stars may host habitable planets with Earth-like atmospheres and biospheres is a major goal in exoplanet research.
We study the origin and escape of catastrophically outgassed volatiles (H2O, CO2) from exomoons with Earth-like densities and masses of 0.1M⊕, 0.5M⊕ and 1M⊕ orbiting an extra-solar gas giant inside the habitable zone of a young active solar-like star.
To sort out the biological intricacies of Earth-like planets, astronomers have developed computer models that examine how ultraviolet radiation from other planets' nearby suns may affect those worlds, according to new research published June 10 in Astrophysical Journal.
By now, observations of exoplanets have found more than 50 binary star systems hosting 71 planets.
Viewed from above, our solar system's planetary orbits around the sun resemble rings around a bulls-eye. Each planet, including Earth, keeps to a roughly circular path, always maintaining the same distance from the sun.
From the numerous detected planets outside the Solar system, no terrestrial planet comparable to our Earth has been discovered so far.
Locating planets in HabitableZones (HZs) around other stars is a growing field in contemporary astronomy.
Young terrestrial planets, when they are still embedded in a circumstellar disk, accumulate an atmosphere of nebula gas.
We present the thermal evolution and emergent spectra of solidifying terrestrial planets along with the formation of steam atmospheres.
The water ice or snow line is one of the key properties of protoplanetary disks that determines the water content of terrestrial planets in the habitable zone.
Priorities in exo-planet research are rapidly moving from finding planets to characterizing their physical properties. Of key importance is their chemical composition, which feeds back into our understanding of planet formation.
Understanding the surface and atmospheric conditions of Earth-size, rocky planets in the habitable zones (HZs) of low-mass stars is currently one of the greatest astronomical endeavors.
Considerable progress has been made in recent years in observations of atmospheric signatures of giant exoplanets, but processes in rocky exoplanets remain largely unknown due to major challenges in observing small planets.
Geological activity is thought to be important for the origin of life and for maintaining planetary habitability. We show that transient sulfate aerosols could be a signature of exoplanet volcanism, and therefore a geologically active world.
We propose a method for observing transiting exoplanets with near-infrared high-resolution spectrometers. We aim to create a robust data analysis method for recovering atmospheric transmission spectra from transiting exoplanets over a wide wavelength range in the near infrared.
We introduce a novel Earth-like planet surface temperature model (ESTM) for habitability studies based on the spatial-temporal distribution of planetary surface temperatures.
A team of astronomers using ground-based telescopes in Hawaii, California, and Arizona recently discovered a planetary system orbiting a nearby star that is only 54 light-years away. All three planets orbit their star at a distance closer than Mercury orbits the sun, completing their orbits in just 5, 15, and 24 days.