Abstract
We present a numerical illumination model to calculate direct as well as diffuse or Hapke scattered radiation scenarios on arbitrary planetary surfaces. This includes small body surfaces such as main belt asteroids as well as e.g., the lunar surface. The model is based on the ray tracing method. This method is not restricted to spherical or ellipsoidal shapes but digital terrain data of arbitrary spatial resolution can be fed into the model. Solar radiation is the source of direct radiation, wavelength-dependent effects (e.g. albedo) can be accounted for. Mutual illumination of individual bodies in implemented (e.g. in binary or multiple systems) as well as self-illumination (e.g. crater floors by crater walls) by diffuse or Hapke radiation. The model is validated by statistical methods. A test is utilized to compare simulated images with DAWN images acquired during the survey phase at small body 4 Vesta and to successfully prove its validity.
Highlights
Reliable prediction or at least estimation of illumination conditions on the surface of planetary bides or small bodies like asteroids or comet cores is essential for mission planning purposes
As solar radiation is in general the major source of energy on the surface of a small, atmosphereless body in space, a simulation suite for calculation of the surface radiative intensity delivers boundary conditions for any thermal model of the surface
Surfaces can be of arbitrary shape, i.e. do not need to be convex but can have edges, bulges, juts and overhangs, consider e.g. (25143) Itokawa Surfaces can have arbitrary spatial resolution, triangles of almost sizes can be handled simultanously in the same data set
Summary
We present a numerical illumination model to calculate direct as well as diffuse or Hapke scattered radiation scenarios on arbitrary planetary surfaces. This includes small body surfaces such as main belt asteroids as well as e.g. the lunar surface. The model is based on the raytracing method. This method is not restricted to spherical or ellipsiodal shapes but digital terrain data of arbitrary spatial resolution can be fed into the model. Mutual illumination of individual bodies in implemented (e.g. in binary or multiple systems) as well as self-illumination (e.g. crater floors by crater walls) by diffuse or Hapke radiation. A χ2 test is undertaken to compare simnulated images with DAWN images acquired during the survey phase at small body 4 Vesta
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