Jeřábková, Tereza: Stellar populations in gravitationally bound systems. - Bonn, 2020. - Dissertation, Rheinische Friedrich-Wilhelms-Universität Bonn.
Online-Ausgabe in bonndoc: https://nbn-resolving.org/urn:nbn:de:hbz:5-59390
@phdthesis{handle:20.500.11811/8534,
urn: https://nbn-resolving.org/urn:nbn:de:hbz:5-59390,
author = {{Tereza Jeřábková}},
title = {Stellar populations in gravitationally bound systems},
school = {Rheinische Friedrich-Wilhelms-Universität Bonn},
year = 2020,
month = aug,

note = {The understanding of how, which, where and when stars form provides important information for the vast majority of astronomical fields. Star-formation has a complex multi-scale physical nature. Stars form in dense sub-parsec regions of molecular clouds, and since the very early stages of their life, their destiny is linked to the complex interplay between magneto-hydro-radiation-transfer-dynamics, stellar evolution and stellar dynamics. At the same time, star-forming regions are inevitably coupled to the galactic gravitational potential and as such are affected by tides and shears. This poses a computational challenge for theoretical investigations pushing technical feasibility to its limit in terms of computational time and the required spatial resolution. Nowadays, front-end facilities allow us to obtain detailed observations of nearby (up to 500pc from the Sun) star-forming regions. While such regions allow us to sample near-to-uniform environmental conditions in terms of cloud density, mass and metallicity, they do not allow us to investigate how star formation proceeds in the full range of diverse environmental conditions that can be found in local galaxies and at all redshifts where the stellar population cannot be resolved. Thus, despite a large and fruitful community effort in this field, we are still lacking a complete and coherent picture of how stars and star-clusters form.
This thesis investigates the physics of star-formation and stellar populations combining theoretical modeling with observations on multiple scales from resolved star-forming regions in the Milky Way through to stellar populations in galaxies reaching to cosmic star-formation. The discovery, my confirmation and theoretical explanation of the existence of three stellar populations in the Orion Nebula Cluster is a clear example of the impact and crucial role played by the stellar dynamics on star and star-cluster formation. Furthermore, the thesis presents the discovery, made possible with the advent of the Gaia space mission, of large scale co-eval filaments of star formation, a new fact posing novel viable constraints for theories of star-formation. Individual star-forming regions (in molecular cloud cores forming at least a few binary stellar systems) are used as building blocks of galaxy-wide stellar populations using the Integrated Galactic Initial Mass Function (IGIMF) theory. The publicly available code, GalIMF, has been co-developed within this thesis to synthesise stellar populations of whole galaxies. This allowed me to compute, for the first time, a large grid of the empirically driven variable galaxy-wide stellar initial mass function for direct comparison with observations. This model and the associated code were used, for example, to construct the cosmic star-formation history with a variable stellar-initial mass function.
The research presented in this thesis was published in four refereed publications led by its author and six refereed publications to which the author provided significantly. This thesis as a whole presents a multi-scale and multi-technique contribution to star-formation and stellar populations and opens novel and original routes for future research.},

url = {http://hdl.handle.net/20.500.11811/8534}
}

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