DLR Portal
Home|Textversion|Imprint|Sitemap|Contact |Deutsch
You are here: Home:Departments:Planetary Physics
Extended Search
News
Institute
Departments
Planetary Geology
Asteroids and Comets
Planetary Sensor Systems
Terahertz- and Infrared Sensors
Planetary Physics
Planetary Geodesy
Extrasolar Planets and Atmospheres
Planning and Common Management
Research
Publications
Offers
Service & Links
Send article to a friendPrint

Modeling interiors of Earth-like bodies...



based on numerical calculations using laboratory data of physical material properties therefore aims at improving our understanding of the origins, evolutions, and current states of planets. In the case of the terrestrial planets and satellites within the solar system the resultant radial profiles of density and related material properties are required to be consistent with geophysical observations and cosmochemical evidence for the likely compositions of crust, mantle and core as obtained from measurements by interplanetary space probes. For terrestrial exoplanets, the numerical models have to be consistent with the observed planetary masses and radii measured from ground-based observations and space missions. Calculated models will be used to derive mass-radius relationships for exoplanets assuming a range of different mineralogical compositions to gain insight in the interior structure and possible bulk compositions of these planets. Furthermore, obtaining scaling laws for key physical and chemical properties will be essential for a better understanding of global planetary processes controlling the general evolution of a planetary body and its astrobiological potential to be life-sustaining.

Mass-radius relationships of solid exoplanets ranging from 1 to 15 times the mass of the Earth.
The solid curves represent chemically homogeneous, self-compressible spheres of the following materials: high-pressure water-ice (blue line), Magnesium-perovskite (red line), and epsilon-Iron (black line). The dashed curves denote differentiated planets of various bulk composition. The red dashed curve is for Earth-like planets with an iron core of 32.6 wt.-% and a 67.5 wt.-% silicate mantle. The blue dashed curve is for ocean planets using the Jovian moon Ganymede as a type-example, resulting in a 45 wt.-% water-ice shell surrounding a 48.5 wt.-% silicate mantle, and a 6.5 wt.-% iron core. The black dashed curve is for iron-rich planets like Mercury composed of a 70 wt.-% iron core overlain by a 30 wt.-% silicate mantle. The triangle indicates the relative position of the Earth. The solid ellipses represent the first low-mass exoplanets with a measured planetary radius and total mass according to their observational uncertainties. Source: F.W. Wagner et al. (2011), Icarus 214, 366-376.

Home
Publications
Theses/ Jobs
Contact
Topics
Interior Structure of Planetary Bodies
Mantle Convection in Planets and Moons
Gravitational and Magnetic Fields
Seismology of Planetary Bodies
Habitability and Thermal Evolution
Tectonics of Planetary Surfaces
Thermal and Physical Modeling of Planetary Surfaces
Thermal Probes for Measuring Surface Heat Flow
Geodynamics Workshop
Home
Website of the Location
Work group "Dynamik des Erdinneren" (German)
Deutsche Geophysikalische Gesellschaft (German)
Helmholtz Alliance "Planetary Evolution and Life"
Institute of Planetary Research
Workgroup Planetary Physics
Related Topics
Lunar and Planetary Science and Exploration
Copyright © 2012 German Aerospace Center (DLR). All rights reserved.