{"id":{"repo_id":"potsdam-thes","oai_identifier":"oai:kobv.de-opus4-uni-potsdam:69560"},"canonical_url":"https://search.dev.ndltd.org/etd/potsdam-thes/oai:kobv.de-opus4-uni-potsdam:69560","repository":{"repo_id":"potsdam-thes","name":"Universität Potsdam - Thes","base_url":"https://publishup.uni-potsdam.de/opus4-ubp/oai"},"display":{"title":"The Impact of realistic galaxy orbits on jellyfish galaxy properties","abstract":"Galaxy clusters, the most massive dark matter halos in the universe, decisively influence their environment and the evolution of galaxies within them. As galaxies move supersonically through the hot, magnetized intracluster medium (ICM) filling the space between galaxies in galaxy clusters, ram pressure stripping (RPS) can remove large fractions of the interstellar and circumgalactic gas of galaxies. This process creates jellyfish galaxies with tails extending up to 100 kpc, and transforms star-forming spirals into quenched galaxies. The multiphase, magnetized and star-forming tails of jellyfish galaxies also serve as unique astrophysical laboratories. Cosmological simulations can model RPS, but their resolution is often too low to capture the detailed physics of jellyfish galaxies. Alternatively, windtunnel simulations, which expose galaxies in their rest frames to a wind that resembles the ICM, allow for a higher resolution but typically rely on idealized wind conditions. In this thesis, I present eight high-resolution windtunnel simulations of RPS for 1e12 M☉ galaxies. I build on the setup from Sparre et al. (2024a) and incorporate realistic ICM-winds derived from galaxy orbits in the cosmological zoom-in simulations PICO-Clusters. I validate the initial conditions using PICO-Clusters, explore simulating the impact of dark matter via a static potential, and optimize the simulation mesh to reduce computational costs. My simulations reveal fragmented jellyfish tails with fountain flows and aligned magnetic fields. The properties of these tails and the efficiency of stripping vary depending on whether galaxies already experience significant ram pressure outside the cluster's virial radius or only after a period of falling in to galaxy clusters, together with material that is accreted onto these clusters and shocked near the cluster's virial radius.","abstract_html":"Galaxy clusters, the most massive dark matter halos in the universe, decisively influence their environment and the evolution of galaxies within them. As galaxies move supersonically through the hot, magnetized intracluster medium (ICM) filling the space between galaxies in galaxy clusters, ram pressure stripping (RPS) can remove large fractions of the interstellar and circumgalactic gas of galaxies. This process creates jellyfish galaxies with tails extending up to 100 kpc, and transforms star-forming spirals into quenched galaxies. The multiphase, magnetized and star-forming tails of jellyfish galaxies also serve as unique astrophysical laboratories. Cosmological simulations can model RPS, but their resolution is often too low to capture the detailed physics of jellyfish galaxies. Alternatively, windtunnel simulations, which expose galaxies in their rest frames to a wind that resembles the ICM, allow for a higher resolution but typically rely on idealized wind conditions. In this thesis, I present eight high-resolution windtunnel simulations of RPS for 1e12 M☉ galaxies. I build on the setup from Sparre et al. (2024a) and incorporate realistic ICM-winds derived from galaxy orbits in the cosmological zoom-in simulations PICO-Clusters. I validate the initial conditions using PICO-Clusters, explore simulating the impact of dark matter via a static potential, and optimize the simulation mesh to reduce computational costs. My simulations reveal fragmented jellyfish tails with fountain flows and aligned magnetic fields. The properties of these tails and the efficiency of stripping vary depending on whether galaxies already experience significant ram pressure outside the cluster's virial radius or only after a period of falling in to galaxy clusters, together with material that is accreted onto these clusters and shocked near the cluster's virial radius.","abstract_has_math":false,"creators":["Dusch, Niklas"],"institution":"Universität Potsdam","degree_name":null,"degree_level":"master","degree_discipline":null,"degree_department":null,"school":null,"contributors":["Puchwein, Ewald","Pfrommer, Christoph","Wisotzki, Lutz"],"advisors":[],"committee_chairs":[],"committee_members":[],"year":2025,"date_issued":"2025-10-24","date_published":"2025-10-24","updated_at":"2026-07-24T03:52:15Z","subjects":["galaxies","jellyfish galaxy","galaxy clusters","magnetohydrodynamics","simulations","Galaxien","Quallengalaxie","Galaxienhaufen","Magnetohydrodynamik","Simulationen"],"languages":[],"rights":["CC-BY - Namensnennung 4.0 International"],"rights_urls":[],"identifier_entries":[]},"links":{"outbound_url":"https://publishup.uni-potsdam.de/frontdoor/index/index/docId/69560","outbound_label":"Repository record","outbound_source":"source_url"},"metadata_groups":[{"id":"people","label":"People","entries":[{"key":"dc:contributor","label":"Contributor","values":["Puchwein, Ewald","Pfrommer, Christoph","Wisotzki, Lutz"]},{"key":"dc:creator","label":"Author","values":["Dusch, Niklas"]}]},{"id":"academic_context","label":"Academic Context","entries":[{"key":"dc:publisher","label":"Institution","values":["Universität Potsdam"]},{"key":"dc:type","label":"Dc Type","values":["masterThesis"]},{"key":"thesis:degree_level","label":"Degree Level","values":["master"]},{"key":"thesis:institution_name","label":"Thesis Institution Name","values":["Universität Potsdam"]}]},{"id":"subjects_keywords","label":"Subjects and Keywords","entries":[{"key":"dc:subject","label":"Dc Subject","values":["galaxies","jellyfish galaxy","galaxy clusters","magnetohydrodynamics","simulations","Galaxien","Quallengalaxie","Galaxienhaufen","Magnetohydrodynamik","Simulationen"]}]},{"id":"language_rights","label":"Language and Rights","entries":[{"key":"dc:rights","label":"Dc Rights","values":["CC-BY - Namensnennung 4.0 International"]}]},{"id":"additional","label":"Additional Metadata","entries":[{"key":"dc:description.abstract","label":"Abstract","values":["Galaxy clusters, the most massive dark matter halos in the universe, decisively influence their environment and the evolution of galaxies within them. As galaxies move supersonically through the hot, magnetized intracluster medium (ICM) filling the space between galaxies in galaxy clusters, ram pressure stripping (RPS) can remove large fractions of the interstellar and circumgalactic gas of galaxies. This process creates jellyfish galaxies with tails extending up to 100 kpc, and transforms star-forming spirals into quenched galaxies. The multiphase, magnetized and star-forming tails of jellyfish galaxies also serve as unique astrophysical laboratories. Cosmological simulations can model RPS, but their resolution is often too low to capture the detailed physics of jellyfish galaxies. Alternatively, windtunnel simulations, which expose galaxies in their rest frames to a wind that resembles the ICM, allow for a higher resolution but typically rely on idealized wind conditions. In this thesis, I present eight high-resolution windtunnel simulations of RPS for 1e12 M☉ galaxies. I build on the setup from Sparre et al. (2024a) and incorporate realistic ICM-winds derived from galaxy orbits in the cosmological zoom-in simulations PICO-Clusters. I validate the initial conditions using PICO-Clusters, explore simulating the impact of dark matter via a static potential, and optimize the simulation mesh to reduce computational costs. My simulations reveal fragmented jellyfish tails with fountain flows and aligned magnetic fields. The properties of these tails and the efficiency of stripping vary depending on whether galaxies already experience significant ram pressure outside the cluster's virial radius or only after a period of falling in to galaxy clusters, together with material that is accreted onto these clusters and shocked near the cluster's virial radius.","Galaxienhaufen, die massereichsten Dunkle Materie Halos des Universums, haben einen entscheidenden Einfluss auf ihre Umgebung und auf Galaxienentwicklung in ihnen. Wenn Galaxien sich supersonisch durch das heiße, magnetisierte Intracluster-Medium (ICM) bewegen, das den Raum zwischen den Galaxien in Galaxienhaufen füllt, kann Abtragung durch Staudruck (engl. ram pressure stripping, RPS) große Teile des interstellaren und zirkumgalaktischen Gases aus Galaxien herauslösen, was Quallengalaxien (engl. jellyfish galaxies) mit Schweifen entstehen lässt, die bis zu 100 kpc ausgedehnt sein können. RPS wandelt mithin sternbildende Spiralgalaxien in erloschene Galaxien um. Zudem sind die magnetisierten und sternbildenden Schweife von Quallengalaxien aus mehreren Phasen ein einzigartiges astrophysikalisches Labor. Während kosmologische Simulationen RPS zwar modellieren können, ist deren Auflösung doch oft zu gering, um die detaillierte Physik von Quallengalaxien zu enthüllen. Alternativ ermöglichen Windtunnelsimulationen, in denen Galaxien in ihren Ruhesystemen einem Wind ausgesetzt werden, der das ICM nachbildet, höhere Auflösungen, sind aber typischerweise auf idealisierte Windmodelle angewiesen. In dieser Arbeit stelle ich einen Satz von acht Windtunnelsimulationen von RPS für 1e12 M☉ Galaxien vor, das den Simulationsaufbau aus Sparre et al. (2024a) mit realistischen ICM-Winden erweitert, die von Galaxienorbits in den kosmologischen zoom-in Simulationen PICO-Clusters abgeleitet wurden. Ich überprüfe die Anfangsbedingungen mithilfe von PICO-Clusters, untersuche das Simulieren des Einflusses dunkler Materie mittels eines statischen Potentials und passe das Simulationsnetz an, um Rechenkosten zu reduzieren. Meine Simulationen zeigen fragmentierte Schweife von Quallengalaxien mit fontänenartigen Gasströmungen und ausgerichteten Magnetfeldern. Die Eigenschaften der Schweife sowie die Effizienz der Materialabtragung variieren abhängig davon, ob Glaxien bereits signifikanten Staudruck außerhalb des Virialradius des Galaxienhaufens erleben oder erst nach einer Periode des gemeinsamen Einfallens in den Galaxienhaufen mit umgebenden Gas, das erst nahe dem Virialradius des Galxienhaufens verdichtet, abgebremst und erwärmt wird."]},{"key":"dc:format.medium","label":"Dc Format Medium","values":["application/pdf"]},{"key":"dc:title","label":"Title","values":["The Impact of realistic galaxy orbits on jellyfish galaxy properties","Der Einfluss realistischer Galaxienorbits auf die Eigenschaften von Quallengalaxien"]}]}],"canonical_facts":{"dc:contributor":["Puchwein, Ewald","Pfrommer, Christoph","Wisotzki, Lutz"],"dc:creator":["Dusch, Niklas"],"dc:description.abstract":["Galaxy clusters, the most massive dark matter halos in the universe, decisively influence their environment and the evolution of galaxies within them. As galaxies move supersonically through the hot, magnetized intracluster medium (ICM) filling the space between galaxies in galaxy clusters, ram pressure stripping (RPS) can remove large fractions of the interstellar and circumgalactic gas of galaxies. This process creates jellyfish galaxies with tails extending up to 100 kpc, and transforms star-forming spirals into quenched galaxies. The multiphase, magnetized and star-forming tails of jellyfish galaxies also serve as unique astrophysical laboratories. Cosmological simulations can model RPS, but their resolution is often too low to capture the detailed physics of jellyfish galaxies. Alternatively, windtunnel simulations, which expose galaxies in their rest frames to a wind that resembles the ICM, allow for a higher resolution but typically rely on idealized wind conditions. In this thesis, I present eight high-resolution windtunnel simulations of RPS for 1e12 M☉ galaxies. I build on the setup from Sparre et al. (2024a) and incorporate realistic ICM-winds derived from galaxy orbits in the cosmological zoom-in simulations PICO-Clusters. I validate the initial conditions using PICO-Clusters, explore simulating the impact of dark matter via a static potential, and optimize the simulation mesh to reduce computational costs. My simulations reveal fragmented jellyfish tails with fountain flows and aligned magnetic fields. The properties of these tails and the efficiency of stripping vary depending on whether galaxies already experience significant ram pressure outside the cluster's virial radius or only after a period of falling in to galaxy clusters, together with material that is accreted onto these clusters and shocked near the cluster's virial radius.","Galaxienhaufen, die massereichsten Dunkle Materie Halos des Universums, haben einen entscheidenden Einfluss auf ihre Umgebung und auf Galaxienentwicklung in ihnen. Wenn Galaxien sich supersonisch durch das heiße, magnetisierte Intracluster-Medium (ICM) bewegen, das den Raum zwischen den Galaxien in Galaxienhaufen füllt, kann Abtragung durch Staudruck (engl. ram pressure stripping, RPS) große Teile des interstellaren und zirkumgalaktischen Gases aus Galaxien herauslösen, was Quallengalaxien (engl. jellyfish galaxies) mit Schweifen entstehen lässt, die bis zu 100 kpc ausgedehnt sein können. RPS wandelt mithin sternbildende Spiralgalaxien in erloschene Galaxien um. Zudem sind die magnetisierten und sternbildenden Schweife von Quallengalaxien aus mehreren Phasen ein einzigartiges astrophysikalisches Labor. Während kosmologische Simulationen RPS zwar modellieren können, ist deren Auflösung doch oft zu gering, um die detaillierte Physik von Quallengalaxien zu enthüllen. Alternativ ermöglichen Windtunnelsimulationen, in denen Galaxien in ihren Ruhesystemen einem Wind ausgesetzt werden, der das ICM nachbildet, höhere Auflösungen, sind aber typischerweise auf idealisierte Windmodelle angewiesen. In dieser Arbeit stelle ich einen Satz von acht Windtunnelsimulationen von RPS für 1e12 M☉ Galaxien vor, das den Simulationsaufbau aus Sparre et al. (2024a) mit realistischen ICM-Winden erweitert, die von Galaxienorbits in den kosmologischen zoom-in Simulationen PICO-Clusters abgeleitet wurden. Ich überprüfe die Anfangsbedingungen mithilfe von PICO-Clusters, untersuche das Simulieren des Einflusses dunkler Materie mittels eines statischen Potentials und passe das Simulationsnetz an, um Rechenkosten zu reduzieren. Meine Simulationen zeigen fragmentierte Schweife von Quallengalaxien mit fontänenartigen Gasströmungen und ausgerichteten Magnetfeldern. Die Eigenschaften der Schweife sowie die Effizienz der Materialabtragung variieren abhängig davon, ob Glaxien bereits signifikanten Staudruck außerhalb des Virialradius des Galaxienhaufens erleben oder erst nach einer Periode des gemeinsamen Einfallens in den Galaxienhaufen mit umgebenden Gas, das erst nahe dem Virialradius des Galxienhaufens verdichtet, abgebremst und erwärmt wird."],"dc:format.medium":["application/pdf"],"dc:publisher":["Universität Potsdam"],"dc:rights":["CC-BY - Namensnennung 4.0 International"],"dc:subject":["galaxies","jellyfish galaxy","galaxy clusters","magnetohydrodynamics","simulations","Galaxien","Quallengalaxie","Galaxienhaufen","Magnetohydrodynamik","Simulationen"],"dc:title":["The Impact of realistic galaxy orbits on jellyfish galaxy properties","Der Einfluss realistischer Galaxienorbits auf die Eigenschaften von Quallengalaxien"],"dc:type":["masterThesis"],"thesis:degree_level":["master"],"thesis:institution_name":["Universität Potsdam"]},"updated_at":"2026-07-24T03:52:15Z"}