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Abstract:

Abstract:
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 in the
system do not gravitationally perturb terrestrial planets outside of
their habitable zone, the orbital region allowing the existence of
liquid water. We quantify the dynamical habitability of 85 known
extrasolar planetary systems via simulations of their orbital dynamics
in the presence of potentially habitable terrestrial planets. When
requiring that habitable planets remain strictly within their
habitable zone at all time, the perturbing influence of giant planets
extends beyond the traditional Hill sphere for close encounters:
terrestrial planet excursions outside of the habitable zone are also
caused by secular eccentricity variations and, in some cases, strong
mean-motion resonances. Our results indicate that more than half the
known extrasolar planetary systems (mostly those with distant,
eccentric giant planets) are unlikely to harbor habitable terrestrial
planets. About 1/4 of the systems (mostly those with close-in giant
planets), including 1/3 of the potential targets for the Terrestrial
Planet Finder, appear as dynamically habitable as our own Solar
System. The influence of yet undetected giant planets in these systems
could compromise their dynamical habitability. Some habitable
terrestrial planets in our simulations have substantial eccentricities
(e > 0.1) which may lead to large seasonal climate variations and thus
affect their habitability.

Comments:

This paper addresses the question of whether an Earth-like planet
would be habitable if it co-existed with some of the eccentric or hot
Jovians discovered over the last decade of exoplanet surveys.

The study is, of course, incomplete since we don't know what other
planets also exist in those systems, some of which may further perturb
or stabilise a planet in the HZ, and it does not cover the question of
whether a habitable planet could have survived the putative migration
of a Jovian to a a hot, close orbit.

However, it clearly scotches the notion that such systems are
intrinsically incapable of harbouring a stable planet in the HZ.