Thermophysical Simulations

Using thermophysical simulations, we calculate the temporal temperature evolution in the near-surface layers of bodies in our solar system, such as planets, asteroids, comets, and (ice) moons. We compare these models with measurement data from space missions and laboratory experiments, allowing us to infer the properties of these layers. This includes, for example, how well celestial bodies near their surfaces can transport heat or how porous (i.e., "holey") they are. In turn, this helps us determine the material composition of the near-surface layers. Altogether, this contributes to a better understanding of how the celestial bodies in our solar system formed and have evolved since their origin.

At the Institute of Planetology, we are developing a versatile numerical thermophysical model (TPM). The model first calculates how much solar heat reaches the surface of a celestial body by taking into account the precise position of the body on its orbit around the Sun, its rotation, and its exact shape, which often deviates significantly from a sphere in the case of small bodies. However, not every part of the surface receives all the radiation it should theoretically get from the Sun. Some regions are at least temporarily in shadow due to large boulders. Other regions receive significantly more radiation because incoming sunlight is reflected multiple times on the surface, concentrating at certain points. Using the model, which solves the heat transport equation, we can determine how the incoming heat is distributed in the near-surface layers and what surface temperatures this ultimately leads to.

This approach works for different types of celestial bodies (rocky ones, such as the Moon or Mercury, or icy ones, such as comets and ice moons). Our thermophysical software is modular in design, allowing the straightforward addition of any desired physical descriptions and processes.