Habitability of Known Exoplanetary Systems Based on Measured Stellar Properties

@article{Jones2006HabitabilityOK,
  title={Habitability of Known Exoplanetary Systems Based on Measured Stellar Properties},
  author={Barrie W. Jones and P. Nick Sleep and David R. Underwood},
  journal={The Astrophysical Journal},
  year={2006},
  volume={649},
  pages={1010 - 1019}
}
Habitable planets are likely to be broadly Earth-like in composition, mass, and size. Masses are likely to be within a factor of a few of the Earth's mass. Currently, we do not have sufficiently sensitive techniques to detect Earth-mass planets, except in rare circumstances. It is thus necessary to model the known exoplanetary systems. In particular, we need to establish whether Earth-mass planets could be present in the classical habitable zone (HZ) or whether the giant planets that we know to… 

Figures and Tables from this paper

Habitability of exoplanetary systems with planets observed in transit

We have used the measured properties of the stars in the 79 exoplanetary systems with one or more planets that have been observed in transit, to estimate each system's present habitability. Such

Habitable zone lifetimes of exoplanets around main sequence stars.

The results show that exoplanet HD 85512b is no longer within the HZ, assuming it has an Earth analog atmosphere, and should be considered in future models of planetary habitability as setting an upper limit on the lifetime of any potential exoplanetary biosphere.

Dynamical Aspects for the Earth’s Habitability

Discoveries of more than 560 extrasolar planets show a huge diversity of these planetary systems. Most of the extrasolar planetary systems are quite different to our solar system, only some of them

M stars as targets for terrestrial exoplanet searches and biosignature detection.

It is concluded that attempts at remote sensing of biosignatures and nonbiological markers from M star planets are important, not as tests of any quantitative theories or rational arguments, but instead because they offer an inspection of the residues from a Gyr-long biochemistry experiment in the presence of extreme environmental fluctuations.

A stability catalogue of the habitable zones in extrasolar planetary systems

In the near future, space missions will be launched (e.g. COROT, KEPLER) to detect Earth-like extrasolar planets. The orbital elements of these (still hypothetic) planets will contain some

FORMATION, TIDAL EVOLUTION, AND HABITABILITY OF THE KEPLER-186 SYSTEM

The Kepler-186 system consists of five planets orbiting an early M dwarf. The planets have physical radii of 1.0–1.50 R⊕ and orbital periods of 4–130 days. The 1.1 R⊕ Kepler-186f with a period of 130

On the detection of (habitable) super-Earths around low-mass stars using Kepler and transit timing variation method

We present the results of an extensive study of the detectability of Earth-sized planets and super-Earths in the habitable zones of cool and low-mass stars using transit timing variation method. We

Formation, Dynamical Evolution, and Habitability of Planets in Binary Star Systems

A survey of currently known planet-hosting stars indicates that approximately 25% of extrasolar planetary systems are within dual-star environments. Several of these systems contain stellar

Planetary Dynamics and Habitable Planet Formation in Binary Star Systems

How our planet was formed, how life came about, and whether life exists elsewhere in the universe are among some of the long-standing questions in human history. The latter, which has been the main

Probability of Finding Terrestrial Planet Within Habitable Zone of Extrasolar Planetary System

Habitable zone in a planetary system is defined as the region around a star where life-supporting planets can exist. Typically it requires the presence of liquid water on the planetary surface.

References

SHOWING 1-10 OF 22 REFERENCES

Prospects for Habitable “Earths” in Known Exoplanetary Systems

We have examined whether putative Earth-mass planets could remain confined to the habitable zones (HZs) of the 111 exoplanetary systems confirmed by 2004 August. We find that in about half of these

Dynamical Habitability of Known Extrasolar Planetary Systems

Habitability is usually defined as the requirement for a terrestrial planet's atmosphere to sustain liquid water. This definition can be complemented by the dynamical requirement that other planets

Statistical properties of exoplanets. III. Planet properties and stellar multiplicity

Among the hundred or so extrasolar planets discovered to date, 19 are orbiting a component of a double or multiple star system. In this paper, we discuss the properties of these planets and compare

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.

Stability of Satellites around Close-in Extrasolar Giant Planets

We investigate the long-term dynamical stability of hypothetical moons orbiting extrasolar giant planets. Stellar tides brake a planet's rotation and, together with tidal migration, act to remove

Habitable planets with high obliquities.

It is shown that a significant fraction of extrasolar Earth-like planets may still be habitable, even if they are subject to large obliquity fluctuations, and that Earth's climate would become regionally severe in such circumstances.

A Reduced Efficiency of Terrestrial Planet Formation following Giant Planet Migration

Substantial orbital migration of massive planets may occur in most extrasolar planetary systems. Since migration is likely to occur after a significant fraction of the dust has been locked up into

Dynamical Stability of Earth‐like Planetary Orbits in Binary Systems

This paper explores the stability of an Earth‐like planet orbiting a solar‐mass star in the presence of an outer‐lying intermediate‐mass companion. The overall goal is to estimate the fraction of

A Dynamical Analysis of the 47 Ursae Majoris Planetary System

Thirteen years of Doppler velocity measurements have revealed the presence of two planets orbiting the star 47 Ursae Majoris on low-eccentricity orbits. A two-Keplerian fit to the radial velocity

Survival of Terrestrial Planets in the Presence of Giant Planet Migration

The presence of "hot Jupiters," Jovian-mass planets with very short orbital periods orbiting nearby main-sequence stars, has been proposed to be primarily due to the orbital migration of planets