
doi: 10.13154/294-8584
In dieser Arbeit werden verschiedene Untersuchungen an magnetohydrodynamischen Modellen von Astrosphären (ASn) präsentiert. Die Schockstrukturen der ASn um vier Sterne, den schnell-laufenden O-Stern \(\lambda\) Cephei, die Sonne, unseren nächsten Nachbarn Proxima Centauri, und den M-Stern LHS 1140, wurden untersucht. Eine Methode zur Projektion von ASn, um künstliche Beobachtungsbilder (kBBr) zu generieren, wurde erarbeitet und auf die oben genannten ASn angewandt. Innerhalb des Modells von \(\lambda\) Cephei wurden verschiedene Störungen vor dem Bugschock injiziert, um deren Auswirkungen auf die Schockstruktur und die kBBr zu untersuchen. Der Einfluss der Relativgeschwindigkeit zwischen Stern und Umgebung wurde anhand des Modells von \(\lambda\) Cephei in sowohl zwei als auch drei Raumdimensionen untersucht. Der Transport kosmischer Strahlung durch die ASn von Proxima Centauri und LHS 1140 wurde in Bezug auf die Habitabilität von erdähnlichen Planeten innerhalb der habitablen Zone des jeweiligen Sterns modelliert.
Within this work, several investigations into magnetohydrodynamic models of astrospheres are presented. The shock structures of the astrospheres around four stars, the runaway O-star \(\lambda\) Cephei, the Sun, our next neighbour Proxima Centauri, and the M-star LHS 1140, were examined. A method of projecting astrospheres to generate synthetic observational images was devised and applied to the aforementioned astrospheres. Within the model of \(\lambda\) Cephei a selection of perturbations has been injected in front of the bow shock in order to analyse their effects on the shock structure and synthetic observational images. The influence of the relative speed between the star and its environment has been evaluated with the model of \(\lambda\) Cephei as a prototype in both two and three spatial dimensions. The transport of cosmic rays through the astrospheres of Proxima Centauri and LHS 1140 has been examined with regard to the habitability of Earth-like planets within the respective star’s habitable zone.
Sternwind, Magnetohydrodynamik, Interstellare Materie, ddc:530, Astrophysik, 530 Physik, Theoretische Physik
Sternwind, Magnetohydrodynamik, Interstellare Materie, ddc:530, Astrophysik, 530 Physik, Theoretische Physik
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