TY - JOUR A1 - Rodener, Daniel A1 - Schäfer, Myriam A1 - Hausmann, Michael A1 - Hildenbrand, Georg T1 - Assessing the Potential for Liquid Solvents from X-ray Sources: Considerations on Bodies Orbiting Active Galactic Nuclei JF - Galaxies N2 - We aim to establish a rough first prospect on the potential of certain biorelevant solvents (water, ammonia, and methane) being present in liquid form inside the uppermost few meters of several modeled rocky and icy surfaces of hypothetical bodies orbiting active galactic nuclei (AGNs) and investigate under which constraints this might occur. For this, we adjust and average X-ray spectra from a sample of 20 Type-1 Seyfert galaxies to calculate the mean snowline of the sample used. We then vary the hypothetical body’s orbit between 10% and 100% of the snowline radius and calculate a sub-surface attenuation within four different model surface compositions for each. We then use this as a continuous source term for a thermal model. Example bodies are systematically investigated with sizes between 1/30 and 20 earth radii, with further variations also considered (such as possible bound rotation), to end up with a perspective of solvent phases under a wide slew of different conditions. We find that liquid solvents are possible under a multitude of parameters, with temperature being the main constraint to liquid water whereas body size and pressure are the main constraint to liquid methane and ammonia. KW - Lösungsmittel KW - Röntgenspektrum Y1 - 2022 U6 - https://doi.org/https://doi.org/10.3390/galaxies10050101 SN - 2075-4434 VL - 10 IS - 5 PB - MDPI AG ER - TY - CHAP A1 - Hildenbrand, Georg A1 - Paschek, Klaus A1 - Schäfer, Myriam A1 - Hausmann, Michael T1 - Cryovolcanism in the Solar System and beyond: Considerations on Energy Sources, Geological Aspects, and Astrobiological Perspectives T2 - Astronomy and Planetary Science - From Cryovolcanism to Black Holes and Galactic Evolution N2 - Volcanism based on melting rocks (silicate volcanism) is long known on Earth and has also been found on Jupiter’s moon Io. Remnants of this type of volcanism have been identified also on other bodies in the solar system. Energy sources powered by accretion and the decay of radioactive isotopes seem to be dominant mainly inside larger bodies, which have enough volume to accumulate and retain this energy in significant amounts. On the other hand, the impact of tidal forces allows even tiny bodies to melt up and pass into the stage of cryovolcanism. The dependence of tidal heating on the size of the object is minor, but the masses of and the distances to accompanying bodies as well as the inner compositions of the heated body are central factors. Even though Io as an example of a body supporting silicate volcanism is striking, the physics of tidal forces might suggest a relatively high probability for cryovolcanism. This chapter aims at considering the parameters known and objects found so far in our solar system to give insights into where in our system and other planetary systems cryovolcanism might be expected. KW - Sonnensystem KW - Vulkanismus Y1 - 2022 SN - 9781803561196 U6 - https://doi.org/https://doi.org/10.5772/intechopen.105067 PB - IntechOpen ER -