This thesis investigates the application of laser-induced breakdown spectroscopy (LIBS) with detection in the vacuum ultraviolet (VUV) spectral range for in-situ space exploration. LIBS is a type of optical emission spectroscopy (OES). For LIBS, a pulsed laser is tightly focused onto the sample, thereby ablating material and exciting a luminous plasma. The atoms and ions contained in the plasma radiate light of characteristic wavelengths, which can be analysed with spectrometers like in other types of OES. The spectral analysis allows to identify the chemical elements in the plasma, which are assumed to be representative for the elements in the sample. With LIBS, in principle all elements can be detected. However, especially the non-metal elements are challenging to detect because their strongest lines are located in the VUV spectral range, i.e. below 200 nm, which is often not investigated. Detection in this range brings its own challenges, since large parts of the radiation spectrum are absorbed by the atmosphere surrounding the sample. On celestial bodies without an atmosphere, such as the Moon, the ambient conditions are well suited for VUV-LIBS analyses. In such a scenario, a better detectability for the otherwise challenging elements C, Cl, H, N, O, P and S is expected compared to LIBS in the usually employed detection range above 200 nm.Motivated by the recent ambitions of the national space agencies to return to the Moon and to potentially set up a permanent moon base in the near future, I investigated the potential of VUV-LIBS in a lunar context. For this project, a dedicated set-up for VUV-LIBS was designed and built at Institut für Optische Sensorsysteme of Deutsches Zentrum für Luft-und Raumfahrt (DLR-OS) in Berlin-Adlershof. After an initial characterization including a relative spectral sensitivity estimate, chemically simple samples have been studied in order to identify emission lines that are typically detectable with this set-up. From these measurements, emission lines from Al,