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Dynamics of the halo gas in disc galaxies

This Thesis studies the dynamics of hot and cold gas outside the plane in galaxies like the Milky-Way (extra-planar gas) and focuses on the interaction between disc and halo material. Stationary models for the cold phase of the
extra-planar gas are presented. They show that the kinematics of this phase must be influenced by the interaction with an ambient medium that we identify as the
hot cosmological corona that surrounds disc galaxies. To study this interaction a novel hydrodynamical code has been implemented and a series of hydrodynamical simulations has been run to investigate the mass and momentum exchange between the cold extra-planar gas clouds and the hot corona. These simulations show that the coronal gas can condense efficiently in the turbulent wakes that form behind the cold clouds and it can be accreted by the disc to sustain star formation. They also predict that the corona cannot be a static structure but it must rotate and
lag by approximately 80-120 km/s with respect to the disc.
Implications of the results of this Thesis for the evolution of star-forming galaxies and for the large-scale dynamics of galactic coronae are also briefly discussed.

Identiferoai:union.ndltd.org:unibo.it/oai:amsdottorato.cib.unibo.it:3743
Date12 April 2011
CreatorsMarinacci, Federico <1983>
ContributorsCiotti, Luca
PublisherAlma Mater Studiorum - Università di Bologna
Source SetsUniversità di Bologna
LanguageEnglish
Detected LanguageEnglish
TypeDoctoral Thesis, PeerReviewed
Formatapplication/pdf
Rightsinfo:eu-repo/semantics/openAccess

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