The pre-transitional disk around the Herbig Ae star HD 169142 shows a complex structure of possible ongoing planet formation in dust thermal emission from the near infrared (IR) to millimeter wavelength range.
Tentative evidence that the properties of evolved stars with planets may be different from what we know for MS hosts has been recently reported.
The study of cosmology, galaxy formation and exoplanetary systems has now advanced to a stage where a cosmic inventory of terrestrial planets may be attempted.
Terrestrial planets formed within gaseous protoplanetary disks can accumulate significant hydrogen envelopes.
Chemical abundance studies of the Sun and solar twins have demonstrated that the solar composition of refractory elements is depleted when compared to volatile elements, which could be due to the formation of terrestrial planets.
The ubiquity of M dwarfs, combined with the relative ease of detecting terrestrial-mass planets around them, has made them prime targets for finding and characterising planets in the "Habitable Zone" (HZ).
Secular and mean motion resonances (hearafter MMR) are effective perturbations to shape planetary systems.
In this paper, we explore how the compositions of terrestrial planets are affected by dynamical evolution of giant planets.
Some recently discovered short-period Earth to Neptune sized exoplanets (super Earths) have low observed mean densities which can only be explained by voluminous gaseous atmospheres.
We present deep Herschel-PACS spectroscopy of far-infrared water lines from a sample of four protoplanetary disks around solar-mass stars, selected to have strong water emission at mid-infrared wavelengths.
The planet, more than four times the mass of the Earth, is one of three that the team detected around a red dwarf star called Wolf 1061.
Life on other planets? A recent study by UNLV astrophysicist Jason Steffen is shedding new light on this persistently challenging question.
Inspired by the close-proximity pair of planets in the Kepler-36 system, we consider two effects that may have important ramifications for the development of life in similar systems where a pair of planets may reside entirely in the habitable zone of the hosting star.
Rotation in planetary atmospheres plays an important role in regulating atmospheric and oceanic heat flow, cloud formation and precipitation.
A terrestrial planet in an orbit far outside of the standard habitable zone could maintain surface liquid water as a result of H2-H2 collision-induced absorption by a thick H2 atmosphere.
The most Earth-like planet could have been made uninhabitable by vast quantities of radiation, new research led by the University of Warwick research has found.
Earth has a unique surface character among Solar System worlds. Not only does it harbor liquid water, but also large continents.
M-dwarf stars are generally considered favourable for rocky planet detection. However, such planets may be subject to extreme conditions due to possible high stellar activity.
A simple metric can be used to determine whether a planet or exoplanet can clear its orbital zone during a characteristic time scale, such as the lifetime of the host star on the main sequence.
The system of four planets around HR8799 offers a unique opportunity to probe the physics and chemistry at play in the atmospheres of self-luminous young (~30 Myr) planets.