HYDROGEN GREENHOUSE PLANETS BEYOND THE HABITABLE ZONE

@article{Pierrehumbert2011HYDROGENGP,
  title={HYDROGEN GREENHOUSE PLANETS BEYOND THE HABITABLE ZONE},
  author={Raymond T. Pierrehumbert and Eric Gaidos},
  journal={The Astrophysical Journal Letters},
  year={2011},
  volume={734}
}
We show that collision-induced absorption allows molecular hydrogen to act as an incondensible greenhouse gas and that bars or tens of bars of primordial H2–He mixtures can maintain surface temperatures above the freezing point of water well beyond the “classical” habitable zone defined for CO2 greenhouse atmospheres. Using a one-dimensional radiative–convective model, we find that 40 bars of pure H2 on a three Earth-mass planet can maintain a surface temperature of 280 K out to 1.5 AU from an… 

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References

SHOWING 1-10 OF 49 REFERENCES

Habitable zones around main sequence stars.

The results suggest that mid-to-early K stars should be considered along with G stars as optimal candidates in the search for extraterrestrial life.

Is Gliese 581d habitable? Some constraints from radiative-convective climate modeling

The recently discovered exoplanet Gl 581d is extremely close to the outer edge of its system’s habitable zone, which has led to much speculation on its possible climate. We have performed a range of

Constraints on the Mass of a Habitable Planet with Water of Nebular Origin

From an astrobiological point of view, special attention has been paid to the probability of habitable planets in extrasolar systems. The purpose of this study is to constrain a possible range of the

ATMOSPHERIC ESCAPE FROM HOT JUPITERS

Photoionization heating from ultraviolet (UV) radiation incidents on the atmospheres of hot Jupiters may drive planetary mass loss. Observations of stellar Lyman-α (Lyα) absorption have suggested

Radiative constraints on the habitability of exoplanets Gliese 581c and Gliese 581d

Aims. The M-type star Gliese 581 is likely to have two super-Earth planets, i.e., Gl 581c and Gl 581d. The present study is to investigate their habitability constrained by radiative properties of

Atmospheres of Protoplanetary Cores: Critical Mass for Nucleated Instability

We systematically study quasi-static atmospheres of accreting protoplanetary cores for different opacity behaviors and realistic planetesimal accretion rates in various parts of the protoplanetary

Enhanced atmospheric loss on protoplanets at the giant impact phase in the presence of oceans

It is suggested that remnants of the noble-gas rich proto-atmosphere survived on Venus, but not on Earth, because most of the neon must have escaped from both planets’ atmospheres later to yield the observed ratio of neon to argon.

Formation of Giant Planets

This is a descriptive and non-mathematical summary of giant planet formation theories. There are two end-member models, core accretion and disk instability. In the core accretion model, several to

Survival of a proto-atmosphere through the stage of giant impacts: the mechanical aspects