Tidal obliquity evolution of potentially habitable planets

@article{Heller2011TidalOE,
  title={Tidal obliquity evolution of potentially habitable planets},
  author={Ren{\'e} Heller and J{\'e}r{\'e}my Leconte and Rory Barnes Leibniz Institute for Astrophysics Potsdam and DFG-funded GrK 1351 and 'ENS Lyon and University of Washington and Seattle and Virtual Planetary Laboratory and Usa},
  journal={Astronomy and Astrophysics},
  year={2011},
  volume={528}
}
Context. Stellar insolation has been used as the main constraint on a planet’s potential habitability. However, as more Earth-like planets are discovered around low-mass stars (LMSs), a re-examination of the role of tides on the habitability of exoplanets has begun. Those studies have yet to consider the misalignment between a planet’s rotational axis and the orbital plane normal, i.e. the planetary obliquity. Aims. This paper considers the constraints on habitability arising from tidal… 

Figures from this paper

Stellar Obliquities in Exoplanetary Systems

The rotation of a star and the revolutions of its planets are not necessarily aligned. This article reviews the measurement techniques, key findings, and theoretical interpretations related to the

Obliquity Variations of Habitable Zone Planets Kepler-62f and Kepler-186f

Obliquity variability could play an important role in the climate and habitability of a planet. Orbital modulations caused by planetary companions and the planet’s spin axis precession due to the

Spin evolution of Earth-sized exoplanets, including atmospheric tides and core–mantle friction

Abstract Planets with masses between 0.1 and 10 M⊕ are believed to host dense atmospheres. These atmospheres can play an important role on the planet's spin evolution, since thermal atmospheric

Tidal locking of habitable exoplanets

Potentially habitable planets can orbit close enough to their host star that the differential gravity across their diameters can produce an elongated shape. Frictional forces inside the planet

The Effect of Post-Newtonian Spin Precessions on the Evolution of Exomoons’ Obliquity

  • L. Iorio
  • Physics, Geology
    The Astronomical Journal
  • 2022
Putative natural massive satellites (exomoons) have gained increasing attention when they orbit Jupiter-like planets within the habitable zone of their host main-sequence star S. An exomoon s is

Exomoon habitability constrained by energy flux and orbital stability

Context. Detecting massive satellites that orbit extrasolar planets has now become feasible, which led naturally to questions about the habitability of exomoons. In a previous study we presented

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

Tidal evolution of planets around brown dwarfs

Context. The tidal evolution of planets orbiting brown dwarfs (BDs) presents an interesting case study because BDs’ terrestrial planet forming region is located extremely close-in. In fact, the

Exomoon habitability and tidal evolution in low-mass star systems

Discoveries of extrasolar planets in the habitable zone (HZ) of their parent star lead to questions about the habitability of massive moons orbiting planets in the HZ. Around low-mass stars, the HZ
...

References

SHOWING 1-10 OF 100 REFERENCES

Tides and the evolution of planetary habitability.

The tidal evolution of hypothetical terrestrial planets around low-mass stars is calculated and it is shown that tides can evolve planets past the inner edge of the habitable zone, sometimes in less than 1 billion years.

HABITABLE CLIMATES: THE INFLUENCE OF OBLIQUITY

Extrasolar terrestrial planets with the potential to host life might have large obliquities or be subject to strong obliquity variations. We revisit the habitability of oblique planets with an energy

HABITABLE CLIMATES: THE INFLUENCE OF ECCENTRICITY

In the outer regions of the habitable zone, the risk of transitioning into a globally frozen “snowball” state poses a threat to the habitability of planets with the capacity to host water-based life.

Habitable planets around the star Gliese 581

Radial velocity surveys are now able to detect terrestrial planets at habitable distance from M-type stars. Recently, two planets with minimum masses below 10 Earth masses were reported in a triple

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 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.

TIDAL LIMITS TO PLANETARY HABITABILITY

The habitable zones (HZs) of main-sequence stars have traditionally been defined as the range of orbits that intercept the appropriate amount of stellar flux to permit surface water on a planet.

Tidal dissipation within hot Jupiters : a new appraisal

Context. Eccentricity or obliquity tides have been proposed as the missing energy source that may explain the anomalously large radius of some transiting “hot Jupiters”. To maintain a non-zero and

Shrinking Binary and Planetary Orbits by Kozai Cycles with Tidal Friction

At least two arguments suggest that the orbits of a large fraction of binary stars and extrasolar planets shrank by 1-2 orders of magnitude after formation: (1) the physical radius of a star shrinks

Tidal heating of terrestrial extrasolar planets and implications for their habitability

The tidal heating of hypothetical rocky (or terrestrial) extrasolar planets spans a wide range of values depending on stellar masses and initial orbits. Tidal heating may be sufficiently large (in
...