## 1 Introduction  
Finding high-power sources with precisely defined parameters that are able to deliver a high amount of energy to an isolated experimental system is a challenging problem for laboratory astrophysics. These experiments involve high-energy states of matter in supernovae explosion shocks [1]), lightning discharges [2; 3; 4; 5; 6; 7], interacting explosions, plasma jets [8], accretion processes [9], inertial fusion [10], the generation of extremely hard radiation [11], asteroid impacts and their consequences to the chemistry of early planets [12; 13; 14; 15], meteor plasmas, and meteor spectra [16; 17; 18; 19; 20]. Laser interaction experiments with meteorites offer a unique opportunity to explore the spectra and the properties of laser-induced plasma (LIP), suitable for the simulation of the physics and chemistry of meteor plasma. The classical application of such studies performed with tabletop (up to J-class lasers) as well as high-power (up to kJ-class lasers) laser sources involves the exploration of hypervelocity atmospheric entry, the effects of asteroid impact, space weathering, and bulk elemental analysis. This idea was originally proposed by [PERSON] and [PERSON] from the US Cornell Aeronautical Laboratory in in 1964 [21]. In the early 1970s, [PERSON] et al. [22] employed laser ablation in the first simulation of impact evaporation, and [PERSON] et al. [23] pioneered the first fundamental description of laser light interaction with targets. Subsequent studies explored the formation of ions and dust particles [24], impact physics [25], hypervelocity damage on spacecraft materials [26], impact melting and the recrystallization of asteroid surfaces [27], space weathering by micrometeorite impacts [28; 29; 30; 31; 32; 33; 34], the weathering of the lunar surface [35; 36], impact ejecta redeposition [37], impact shock wave propagation in materials [38], distribution, mineralogy, and the composition of ejecta produced by the high-velocity collisions of planetary bodies [39; 40], the surface structures and reflectance properties of regoliths produced by space weathering [41], the crater-like structures formed after the laser shot [42], or the transformation of carbonates in terrestrial impact craters [43]. The chemical consequences of an impact event were explored in 1989 by a group led by [PERSON] and [PERSON] [44]. Using laboratory lasers with energy up to 1 J, they estimated the yields of molecules formed by impact-induced atmosphere transformation [45]. [PERSON] et al. [46] explored the synthesis of more complex organic substances, [PERSON] et al. [47; 48] demonstrated impact-induced chemical synthesis on icy bodies, and [PERSON] et al. [49] explored the impact-assisted synthesis of nitrates on early Mars. Our current study focuses on the morphology of meteorite ablated surfaces. However, the same kJ-TW-class high-power PALS laser [50] was employed for the first time in research focused on asteroid impact chemical consequences almost 20 years ago. Simulations by PALS demonstrated the impact synthesis of amino acids [51], canonical nucleobases [13; 14; 52; 53; 54], and sugars [55]. They also helped to explore the transformation of simple molecules occurring on early terrestrial planets [56], such as formamide [57], isocyanic acid [58], hydrogen cyanide [15], acetylene [59], methane [60], or carbon monoxide [56; 61]. In addition to laboratory astrophysics, lasers are or will be applied in many space technologies (reviewed in [62] and references therein) for the in situ exploration and prospection of asteroids, comets, space debris mitigation, propelling space vehicles, or for the deflection of potentially dangerous near-Earth objects [63; 64; 65; 66; 67]. For their development, laboratory interaction experiments are crucial because the ablation process is significantly influenced by physical/chemical matrix effects. The ablation behavior of minerals common on asteroids has already been the subject of several scientific studies [68; 69; 70].