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Habitable Zones & Global Climate: June 2019


Low-gravity waterworlds (M≲0.1M⊕) are of interest for their potential habitability. The weakly bound atmospheres of such worlds have proportionally larger radiative surfaces and are more susceptible to escape.

The main idea is easy to grasp: Set Goldilocks loose in our galaxy and let her choose a planet that's "just right." For decades, the Goldilocks zone has been the go-to shorthand for scientists. More formally known as the "habitable zone," it's the region around a star where the temperature is just right for liquid water to pool on the surface of planets with suitable atmospheres.

High-energy radiation caused by exoplanetary space weather events from planet-hosting stars can play a crucial role in conditions promoting or destroying habitability in addition to the conventional factors.

New instruments and telescopes, such as SPIRou, CARMENES and TESS, will increase manyfold the number of known planets orbiting M dwarfs.

Planets in the "Habitable Zones" around M-type stars are important targets for characterization in future observations.

Thousands of exoplanets have been detected to date, and with future planned missions this tally will increase.

A new study from researchers at the Woods Hole Oceanographic Institution (WHOI) and Harvard University may help settle a long-standing question--how small amounts of organic carbon become locked away in rock and sediments, preventing it from decomposing.

Planets similar to Earth - but slightly more irradiated - are expected to enter into a runaway greenhouse state, where all surface water rapidly evaporates, forming an optically thick H2O-dominated atmosphere.

Orbital phase-dependent variations in thermal emission and reflected stellar energy spectra can provide meaningful constraints on the climate states of terrestrial extrasolar planets orbiting M dwarf stars.

The Gaia hypothesis postulates that life regulates its environment to be favorable for its own survival. Most planets experience numerous perturbations throughout their lifetimes such as asteroid impacts, volcanism, and the evolution of a star's luminosity

We investigate the hypothesis that the size of the habitable zone around hardened binaries in dense star-forming regions increases. Our results indicate that this hypothesis is essentially incorrect.