Topography of (exo)planets
arXiv:1902.00047 · doi:10.1093/mnras/sty3253
Abstract
Current technology is not able to map the topography of rocky exoplanets, simply because the objects are too faint and far away to resolve them. Nevertheless, indirect effect of topography should be soon observable thanks to photometry techniques, and the possibility of detecting specular reflections. In addition, topography may have a strong effect on Earth-like exoplanet climates because oceans and mountains affect the distribution of clouds \citep{Houze2012}. Also topography is critical for evaluating surface habitability \citep{Dohm2015}. We propose here a general statistical theory to describe and generate realistic synthetic topographies of rocky exoplanetary bodies. In the solar system, we have examined the best-known bodies: the Earth, Moon, Mars and Mercury. It turns out that despite their differences, they all can be described by multifractral statistics, although with different parameters. Assuming that this property is universal, we propose here a model to simulate 2D spherical random field that mimics a rocky planetary body in a stellar system. We also propose to apply this model to estimate the statistics of oceans and continents to help to better assess the habitability of distant worlds.
References in corpus (9)
- Exoplanet Atmospheres
- A ground-based transmission spectrum of the super-Earth exoplanet GJ1214b
- Inference of Inhomogeneous Clouds in an Exoplanet Atmosphere
- Gliese 581d is the first discovered terrestrial-mass exoplanet in the habitable zone
- A combined transmission spectrum of the Earth-sized exoplanets TRAPPIST-1 b and c
- Exploring the faint young Sun problem and the possible climates of the Archean Earth with a 3-D GCM
- Climate instability on tidally locked exoplanets
- Possible climates on terrestrial exoplanets
- Multifractal topography of several planetary bodies in the Solar System