Paschek, K.; Roßmann, A.; Hausmann, M.; Hildenbrand, G. Analysis of Tidal Accelerations in the Solar System and in Extrasolar Planetary Systems. Appl. Sci.2021, 11, 8624.
Paschek, K.; Roßmann, A.; Hausmann, M.; Hildenbrand, G. Analysis of Tidal Accelerations in the Solar System and in Extrasolar Planetary Systems. Appl. Sci. 2021, 11, 8624.
Paschek, K.; Roßmann, A.; Hausmann, M.; Hildenbrand, G. Analysis of Tidal Accelerations in the Solar System and in Extrasolar Planetary Systems. Appl. Sci.2021, 11, 8624.
Paschek, K.; Roßmann, A.; Hausmann, M.; Hildenbrand, G. Analysis of Tidal Accelerations in the Solar System and in Extrasolar Planetary Systems. Appl. Sci. 2021, 11, 8624.
Abstract
Volcanism powered by tidal forces inside celestial bodies can provide enough energy to keep important solvents for living systems in the liquid phase. Moreover, tidal forces and their environmental consequences may strongly influence habitability of planets and other celestial bodies and may result in special forms of live and living conditions. A prerequisite to calculate such tidal interactions and consequences is depending on simulations for tidal accelerations in a multi-body system. Unfortunately, from measurements in many extrasolar planetary systems only few physical and orbital parameters are well enough known for investigated celestial bodies. For calculating tidal acceleration vectors under missing most orbital parameter exactly, a simulation method is developed that is only based on a few basic parameters, easily measurable even in extrasolar planetary systems. Such a method as being presented here, allows finding a relation between the tidal acceleration vectors and potential heating inside celestial objects. Using values and results of our model approach to our solar system as a “gold standard” for feasibility allowed us to classify this heating in relation to different forms of volcanism. This “gold standard” approach gave us a classification measure for the relevance of tidal heating in other extrasolar systems with a reduced availability of exact physical parameters. We would help to estimate conditions for the identification of potential candidates for further sophisticated investigations by more complex established methods like viscoelastic multi-body theories. As a first example, we applied the procedures developed here to the extrasolar planetary system TRAPPIST-1 as an example to check our working hypothesis.
Copyright:
This is an open access article distributed under the Creative Commons Attribution License which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
