The influence of Jupiter, Mars and Venus on Earth's orbital evolution

• Published in: arXiv.org 2017-08
• Main Authors: Horner, Jonathan, Gilmore, James B, Waltham, Dave
• Format: Article
• Language: English
• Subjects: Climate; Computer architecture; Extrasolar planets; Glacial periods; Habitability; Jupiter; Luminosity; Mars; Orbital mechanics; Planet detection; Planetary evolution; Planetary systems; Solar system; Terrestrial planets; Venus
• ISSN: 2331-8422

In the coming years, it is likely that the first potentially Earth-like planets will be discovered orbiting other stars. Once found, the characterisation of those planets will play a vital role in determining which will be chosen as the first targets for the search for life beyond the Solar System. We must thus be able to gauge the relative importance of the various factors proposed to influence potential planetary habitability, in order to best focus that search. One of the plethora of factors to be considered in that process is the climatic variability of the exo-Earths in question. In the Solar System, the Earth's long-term climate is driven by several factors, including the modifying influence of life on our atmosphere, and the temporal evolution of solar luminosity. The gravitational influence of the other planets in the Solar System adds an extra complication, driving the Milankovitch cycles that are thought to have caused the on-going series of glacial and interglacial periods that have dominated Earth's climate for the past few million years. Here we present preliminary results of three suites of integrations that together examine the influence of Solar System architecture on the Earth's Milankovitch cycles. We consider separately the influence of the planets Jupiter, Mars and Venus, each of which contributes to the forcing of Earth's orbital evolution. Our results illustrate how small changes to the architecture of a given planetary system can result in marked changes in the potential habitability of the planets therein, and are an important first step in developing a means by which the nature of climate variability on planets beyond our Solar System can be characterised.