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Thèses sur le sujet « Bar formation, galaxy evolution »

Auteur : Grafiati

Publié le 9 mars 2023

Mis à jour le 31 juillet 2025

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1

FANALI, ROSSELLA. "Bar-formation as driver of gas inflows in isolated disc galaxies." Doctoral thesis, Università degli Studi di Milano-Bicocca, 2015. http://hdl.handle.net/10281/96384.

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Stellar bars are a common feature in massive disc galaxies. On a theoretical ground, the response of gas to a bar is generally thought to cause nuclear starbursts and, possibly, AGN activity once the perturbed gas reaches the central super-massive black hole. By means of high resolution numerical simulations we detail the purely dynamical effects that a forming bar exerts on the gas of an isolated disc galaxy. The galaxy is initially unstable to the formation of non-axisymmetric structures, and within 1 Gyr it develops spiral arms that eventually evolve into a central stellar bar on kpc scale.

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2

Kraljic, Katarina. "Links between galaxy evolution, morphology and internal physical processes." Thesis, Paris 11, 2014. http://www.theses.fr/2014PA112286/document.

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Cette thèse a pour but de faire le lien entre l’évolution des galaxies, leur morphologie et les processus physiques internes, notamment la formation stellaire comme le résultat du milieu interstellaire turbulent et multiphase, en utilisant les simulations cosmologiques zoom-in, les simulations des galaxies isolées et en interaction, et le modèle analytique de la formation stellaire. Dans le chapitre 1, j’explique la motivation pour cette thèse et je passe brièvement en revue le contexte nécessaire lié à la formation des galaxies et la modélisation en utilisant les simulations numériques. Tout

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3

Williams, Michael J. "Early-type disk galaxies." Thesis, University of Oxford, 2011. http://ora.ox.ac.uk/objects/uuid:936168ab-f49a-410a-9e1b-80c7ad7cf556.

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In this thesis I investigate the dynamics and stellar populations of a sample of 28 edge-on early-type (S0--Sb) disk galaxies, 22 of which host a boxy or peanut-shaped bulge. I begin by constructing mass models of the galaxies based on their observed photometry and stellar kinematics. Subject to cosmologically motivated assumptions about the shape of dark haloes, I measure in a purely dynamical way their stellar and dark masses. I make a preliminary comparison between the dynamically determined stellar masses and those predicted by stellar population models. I then compare the Tully-Fisher (lu

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4

Croton, Darren. "Galaxy Formation and Evolution." Diss., lmu, 2005. http://nbn-resolving.de/urn:nbn:de:bvb:19-44059.

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5

Thomas, Daniel. "Chemical evolution and galaxy formation." Diss., lmu, 2000. http://nbn-resolving.de/urn:nbn:de:bvb:19-4637.

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6

Romano, Donatella. "Chemical evolution and galaxy formation." Doctoral thesis, SISSA, 2002. http://hdl.handle.net/20.500.11767/4041.

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Following a review of the basic ingredients necessary for constructing models of galactic chemical evolution, with a special emphasis on the issue of stellar evolution and nucleosynthesis (which is treated in detail in Chapter 2), I continue with the basic equations that one needs to solve in order to follow the chemical evolution of a system of gas and stars in time and space. The assumptions of the models I have handled with the aim of addressing different aspects of the formation and evolution of the Milky Way and elliptical galaxies are discussed in Chapter 3. In Chapters 4 and 5,

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7

Linke, Laila Maria [Verfasser]. "Testing models of galaxy formation and evolution with galaxy-galaxy-galaxy lensing / Laila Maria Linke." Bonn : Universitäts- und Landesbibliothek Bonn, 2021. http://d-nb.info/1235524469/34.

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8

Burton, Christopher Steven. "The environmental dependence of galaxy evolution." Thesis, University of Hertfordshire, 2013. http://hdl.handle.net/2299/12572.

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Observations of galaxy environments have revealed numerous correlations associated with their intrinsic properties. It is therefore clear that if we are to understand the processes by which galaxies form and evolve, we have to consider the role of their immediate environment and how these trends change across cosmic time. In this thesis, I investigate the relationship between the environmental densities of galaxies and their associated properties by developing and implementing a novel approach to measuring galaxy environments on individual galaxy scales with Voronoi tessellations. Using optica

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9

Moustakas, John. "Spectral Diagnostics of Galaxy Evolution." Diss., The University of Arizona, 2006. http://hdl.handle.net/10150/305142.

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Despite considerable progress in recent years, a complete description of the physical drivers of galaxy formation and evolution remains elusive, in part because of our poor understanding of star formation, and how star formation in galaxies is regulated by feedback from supernovae and massive stellar winds. Insight into the star formation histories of galaxies, and the interplay between star formation and feedback, can be gained by measuring their chemical abundances, which until recently has only been possible for galaxies in the nearby universe. However, reliable star formation and abundance

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10

Bothwell, Matthew Stuart. "Galaxy evolution : near and far." Thesis, University of Cambridge, 2011. https://www.repository.cam.ac.uk/handle/1810/265602.

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The formation of stars from interstellar gas is the cornerstone of galaxy evolution. This thesis represents work undertaken in order to characterise the role of cool interstellar gas, and its relation to star formation, in galaxy evolution across cosmic time. In particular, it concentrates on star forming galaxies at the extremes of the galaxy assembly spectrum - extremely faint dwarfs, and extremely luminous starbursts - in an attempt to test the limits of galaxy evolution models. The thesis falls into two complimentary halves, addressing topics in the low redshift and high redshift Universe

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11

Wijesinghe, Dinuka. "Galaxy star formation rates and their relation to galaxy environments." Thesis, The University of Sydney, 2012. https://hdl.handle.net/2123/28926.

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This thesis investigates various methods of dust obscuration measurements in order to derive accurate SFRs which I then use to investigate the SFR-density relation. I present self-consistent star formation rates derived through pan-spectral analysis of galaxies drawn from the Galaxy and Mass Assembly (GAMA) survey. I determine the most appropriate form of dust obscuration correction via application of a range of extinction laws drawn from the literature as applied to Ha, [On] and UV luminosities. I consider several different obscuration curves, including those of Milky Way, Calzetti (2001) a

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12

Guo, Qi. "Galaxy formation and evolution in a LamdaCDM universe." kostenfrei, 2009. http://edoc.ub.uni-muenchen.de/10678/.

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13

Kitzbichler, Manfred G. "Galaxy formation and evolution in the Millennium Simulation." Diss., lmu, 2008. http://nbn-resolving.de/urn:nbn:de:bvb:19-95401.

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14

Guo, Qi. "Galaxy Formation and Evolution in a LCDM Universe." Diss., lmu, 2009. http://nbn-resolving.de/urn:nbn:de:bvb:19-106781.

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15

Cole, Shaun. "Evolution of large scale structure and galaxy formation." Thesis, University of Cambridge, 1989. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.315745.

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16

Prema, Paresh. "Galaxy formation and evolution using the virtual observatory." Thesis, University of Cambridge, 2009. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.611697.

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17

Maeda, Fumiya. "Mechanisms of Star Formation Suppression in the Strongly Barred Galaxy NGC1300." Doctoral thesis, Kyoto University, 2021. http://hdl.handle.net/2433/263474.

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18

Laine, J. (Jarkko). "Understanding the formation and evolution of disc break features in galaxies." Doctoral thesis, University of Oulu, 2016. http://urn.fi/urn:isbn:9789526213040.

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Abstract The discs in galaxies are radially extended, rotationally supported, ﬂattened systems. In the cosmological Lambda Cold Dark Matter model the formation of the discs is intimately connected with galaxy formation. Generally it is assumed that the discs have exponentially decreasing stellar surface brightness proﬁles, but completely satisfactory theoretical explanation for this has not been presented. Large number of studies in the past decade have challenged this view, and have found a change in the slope of the surface brightness proﬁle in the outer regions of many galaxies discs: the

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19

Bell, Eric Findlay. "Exploring the star formation histories of galaxies." Thesis, Durham University, 1999. http://etheses.dur.ac.uk/4796/.

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In this thesis, I explore the star formation histories of both spiral and elliptical galaxies. In Part 1,1 present an in-depth study of the star formation histories of spiral galaxies with a wide range of properties. Optical and near-infrared colours are used in conjunction with up-to-date stellar population synthesis models to constrain the ages and metallicities of my sample galaxies. I find that age and metallicity gradients are common in spiral galaxies of all types. The age of a spiral galaxy correlates mainly with its surface brightness, and its metallicity correlates strongly with both

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20

FUMAGALLI, MICHELE. "Food for stars: The role of hydrogen in the formation and evolution of galaxies." Doctoral thesis, University of California Santa Cruz, 2012. http://hdl.handle.net/10281/280709.

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The current cosmological model, the Lambda CDM theory, describes with remarkable precision the assembly and growth of the large scale structures and of the dark matter halos in our Universe. A comprehensive theory for the baryon processes that take place within dark matter halos is, instead, still the subject of active research. The three major ingredients of this theory are known: accretion of hydrogen from the intergalactic medium, star formation, and feedback mechanisms in the form of galactic winds. However, the recipe to blend them together has not yet been found. This thesis focuses on t

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21

Ruggiero, Rafael. "Galaxy Evolution in Clusters." Universidade de São Paulo, 2018. http://www.teses.usp.br/teses/disponiveis/14/14131/tde-14022019-140755/.

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In this thesis, we aim to further elucidate the phenomenon of galaxy evolution in the environment of galaxy clusters using the methodology of numerical simulations. For that, we have developed hydrodynamic models in which idealized gas-rich galaxies move within the ICM of idealized galaxy clusters, allowing us to probe in a detailed and controlled manner their evolution in this extreme environment. The main code used in our simulations is RAMSES, and our results concern the changes in gas composition, star formation rate, luminosity and color of infalling galaxies. Additionally to processes ta

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22

Twite, Joanathan W. "Galaxy star formation and mass growth since z=3." Thesis, University of Nottingham, 2016. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.718862.

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In this thesis we investigate the evolution of galaxies since z = 3. There are several methods to measure the star formation rate (SFR) of galaxies, they all however have drawbacks. Several studies have investigated the SFR at high redshifts using SFR tracers that suffer from uncertainties, either from the tracer used, or from the uncertainties correcting for the effects of dust. We have new measurements of the Ha emission line for a sample of galaxies at =~1; Ha is a more accurate SFR-tracer than other commonly used tracers, but until now had been technically difficult to measure at : > 0.8

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23

Majewski, Steven R., Ricardo P. Schiavon, Peter M. Frinchaboy, et al. "The Apache Point Observatory Galactic Evolution Experiment (APOGEE)." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/625493.

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The Apache Point Observatory Galactic Evolution Experiment (APOGEE), one of the programs in the Sloan Digital Sky Survey III (SDSS-III), has now completed its systematic, homogeneous spectroscopic survey sampling all major populations of the Milky Way. After a three-year observing campaign on the Sloan 2.5 m Telescope, APOGEE has collected a half million high-resolution (R similar to 22,500), high signal-to-noise ratio (>100), infrared (1.51-1.70 mu m) spectra for 146,000 stars, with time series information via repeat visits to most of these stars. This paper describes the motivations for the

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24

Clay, Scott Jonathan. "The formation and evolution of dust in semi-analytic models of galaxy formation." Thesis, University of Sussex, 2017. http://sro.sussex.ac.uk/id/eprint/70546/.

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The formation and evolution of galaxies is an interesting subject to study because it incorporates astrophysics from all scales, from the initial perturbations in the early universe creating the large scale structures that produce galaxies, right down to the evolution of stellar populations and their manipulation of the host galaxy. Simulations of galaxy formation allow us to test the various physical recipes against that which is observed in order to build a true and proper picture of what is happening in the real universe. L-Galaxies is a semi-analytic model of galaxy formation built on top

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25

Bird, Jonathan C. "The Formation and Evolution of Disk Galaxies." The Ohio State University, 2012. http://rave.ohiolink.edu/etdc/view?acc_num=osu1345571232.

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26

Impey, C. D., and G. D. Bothun. "MALIN: A Quiescent Disk Galaxy|MALIN 1: A Quiescent Disk Galaxy." Steward Observatory, The University of Arizona (Tucson, Arizona), 1988. http://hdl.handle.net/10150/623912.

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We present new optical and radio spectroscopic observations of the remarkable galaxy Malin 1. This galaxy has unique features that include an extremely low surface brightness disk with an enormous mass of neutral hydrogen, and a low luminosity Seyfert nucleus. Malin 1 is exceptional in its values of MHO, LB, and MHI /Ln, and modest in its surface mass density of gas and stars. Spirals with large Min /LB tend to have low mean column densities of HI, and are close to the threshold for star formation due to instabilities in a rotating gas disk. In these terms, Malin 1 has a disk with extrem

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27

Lo, Faro Barbara. "Physical modelling of high redshift galaxy spectra: a new multiwavelenght view on galaxy formation and evolution." Doctoral thesis, Università degli studi di Padova, 2013. http://hdl.handle.net/11577/3423456.

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A major step forward in our understanding of the formation mechanism and evolution with cosmic time of galaxies is given by the recent development of powerful astronomical tools able to detect exceedingly faint signals from remote distances. One of the latter developments of particular signicance was the opening of wavelengths longwards the classical visual band to the astronomical observation from space. From the mid '80 with the pioneering IRAS survey, until today, with the operation of the Herschel Space Observatory in the far-infrared and the Large Atacama Millimetre Array (ALMA) in the

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28

Duong, Ly. "Unravelling the evolution of the Galactic stellar disk and bulge." Phd thesis, Canberra, ACT : The Australian National University, 2018. http://hdl.handle.net/1885/149502.

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The formation and evolution of spiral galaxies is a research topic central to modern Astronomy. In this context, the Milky Way offers a unique opportunity for astronomers to study a spiral galaxy in detail and thus informs many aspects of galaxy formation theory. The observational signatures of Galactic stellar components provide clues to its assembly history. This thesis is focused on two main components of the Galaxy: the stellar disk and bulge. In particular, we examine the chemical properties of these components and their implications for

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29

McKinnon, Ryan Michael. "Numerically modeling the evolution of dust grains in galaxy formation simulations." Thesis, Massachusetts Institute of Technology, 2019. https://hdl.handle.net/1721.1/123346.

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This electronic version was submitted by the student author. The certified thesis is available in the Institute Archives and Special Collections.<br>Thesis: Ph. D., Massachusetts Institute of Technology, Department of Physics, 2019<br>Cataloged from student-submitted PDF version of thesis.<br>Includes bibliographical references (pages 239-254).<br>In this thesis, I present the development of various models for dust physics suited for galaxy formation simulations. I begin by introducing a model to evolve the spatial distribution of dust in galaxies, with dust treated as a passive scalar advecte

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30

Tyler, Krystal D. "Star Formation and Galaxy Evolution in Different Environments, from the Field to Massive Clusters." Diss., The University of Arizona, 2012. http://hdl.handle.net/10150/265395.

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This thesis focuses on how a galaxy's environment affects its star formation, from the galactic environment of the most luminous IR galaxies in the universe to groups and massive clusters of galaxies. Initially, we studied a class of high-redshift galaxies with extremely red optical-to-mid-IR colors. We used Spitzer spectra and photometry to identify whether the IR outputs of these objects are dominated by AGNs or star formation. In accordance with the expectation that the AGN contribution should increase with IR luminosity, we find most of our very red IR-luminous galaxies to be dominated b

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31

Henriques, Bruno M. "Hybrid galaxy evolution modelling : Monte Carlo Markov Chain parameter estimation in semi-analytic models of galaxy formation." Thesis, University of Sussex, 2010. http://sro.sussex.ac.uk/id/eprint/2334/.

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We introduce a statistical exploration of the parameter space of the Munich semi-analytic model built upon the Millennium dark matter simulation. This is achieved by applying a Monte Carlo Markov Chain (MCMC) method to constrain the 6 free parameters that define the stellar mass function at redshift zero. The model is tested against three different observational data sets, including the galaxy K-band luminosity function, B −V colours, and the black hole-bulge mass relation, to obtain mean values, confidence limits and likelihood contours for the best fit model. We discuss how the model paramet

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32

Franck, Jay. "IDENTIFYING PROTOCLUSTERS IN THE HIGH REDSHIFT UNIVERSE AND MAPPING THEIR EVOLUTION." Case Western Reserve University School of Graduate Studies / OhioLINK, 2018. http://rave.ohiolink.edu/etdc/view?acc_num=case1501165130716782.

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33

Hayes, Christian R., Steven R. Majewski, Matthew Shetrone, et al. "Disentangling the Galactic Halo with APOGEE. I. Chemical and Kinematical Investigation of Distinct Metal-poor Populations." IOP PUBLISHING LTD, 2018. http://hdl.handle.net/10150/626539.

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We find two chemically distinct populations separated relatively cleanly in the [Fe/H]-[Mg/Fe] plane, but also distinguished in other chemical planes, among metal-poor stars (primarily with metallicities [Fe/H] < -0.9) observed by the Apache Point Observatory Galactic Evolution Experiment (APOGEE) and analyzed for Data Release 13 (DR13) of the Sloan Digital Sky Survey. These two stellar populations show the most significant differences in their [X/Fe] ratios for the alpha-elements, C+N, Al, and Ni. In addition to these populations having differing chemistry, the low metallicity high-Mg populat

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34

ZOLDAN, ANNA. "On the Role of Cold Gas in Galaxy Evolution." Doctoral thesis, Università degli Studi di Trieste, 2018. http://hdl.handle.net/11368/2918756.

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My PhD thesis is focused on the role of cold gas in galaxy evolution. The main tools I have used for my research are state-of-the- art semi-analytic models (SAMs), coupled to high-resolution N-body simulations of cosmological volumes. In the first part of my thesis, I analyze results from six different SAMs, all based on the same cosmological simulation, against the latest observational data on the neutral hydrogen (HI) content of galaxies in the local Universe. Only one of the models considered includes a self-consistent partition of the cold gas into HI and molecular hydrogen (H2), and a sta

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Susa, Hajime. "The Thermal Evolution of Primordial Gas Clouds : A clue to galaxy formation." 京都大学 (Kyoto University), 1997. http://hdl.handle.net/2433/202430.

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Dias, Bruno Moreira de Souza. "Formation and evolution of globular clusters in the Galaxy and Magellanic Clouds." Universidade de São Paulo, 2014. http://www.teses.usp.br/teses/disponiveis/14/14131/tde-26082014-090039/.

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Globular clusters are tracers of the formation and evolution of their host galaxies. Kinematics, chemical abundances, age and position of the clusters allows tracing interactions between Milky Way and surrounding galaxies and outlines their chemical enrichment history. In this thesis we analyse mid-resolution spectra of about 800 red giant stars in 51 Galactic globular clusters. It is the first time that [Fe/H] and [Mg/Fe] derived in a consistent way are published for such a huge sample of globular clusters, almost 1/3 of the total number of catalogued clusters. Our metallicities are showed to

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Wong, Oiwei Ivy. "Star formation and galaxy evolution of the local universe based on HIPASS /." Connect to thesis, 2007. http://eprints.unimelb.edu.au/archive/00004069.

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Christlein, Daniel. "Disentangling luminosity, morphology, star formation, stellar mass, and environment in galaxy evolution." Diss., The University of Arizona, 2004. http://hdl.handle.net/10150/280595.

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We present a study of the photometric and spectroscopic properties of galaxies in a sample of six nearby, rich galaxy clusters. We examine the variations of fundamental galaxy properties, such as luminosity, morphology, and star formation rates with environment, providing new constraints on the mechanisms that drive the evolution of galaxies. This study also introduces a new maximum likelihood algorithm to recover the true distribution function of galaxies from an incomplete sample. This algorithm is ideally suited for modern-day surveys that gather a large amount of information about each obj

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Citro, Annalisa <1987&gt. "Investigating the conclusive phases of galaxy evolution: from star formation to quiescence." Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2018. http://amsdottorato.unibo.it/8510/7/tesi_16mar18.pdf.

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Despite the progress made towards a more comprehensive knowledge of galaxy evolution, a global picture of the mechanisms regulating the formation of stars in galaxies, of how galaxy evolutionary properties correlate with stellar masses and star formation rates (SFRs) and of the processes suppressing the star formation in galaxies and their timescales is still lacking. In this thesis work, we attempt to address some of these open questions, inspecting galaxy evolution back in cosmic time. In particular, we start from the archaeological analysis of passive local galaxies (1), reconstructing the

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Simha, Vimal. "Dark Matter Substructures and Galaxy Assembly." The Ohio State University, 2011. http://rave.ohiolink.edu/etdc/view?acc_num=osu1313085907.

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Dimauro, Paola. "Investigating the link between bulge growth and quenching in massive galaxies through polychromatic bulge-disk decompositions in the CANDELS fields." Thesis, Paris Sciences et Lettres (ComUE), 2017. http://www.theses.fr/2017PSLEO011/document.

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Les galaxies passives présentent des morphologies et propriétés structurelles différentes des galaxies de masse similaire formant des étoiles. La preuve d'une distribution bimodale dans propriétés des galaxies suggère un lien entre les processus de quenching et les structures des galaxies. Contraindre les mécanismes et la chronologie de la formation du bulbe s'avère fondamental pour comprendre l'origine de cette corrélation. Les bulbes grossissent-ils au cours de la séquence principale? Les galaxies ré-accrètent-elles un disque formant des étoiles? Les galaxies stoppent-elles leur formation d'

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Andrews, Brett H. "Decoding Galaxy Evolution with Gas-phase and Stellar Elemental Abundances." The Ohio State University, 2014. http://rave.ohiolink.edu/etdc/view?acc_num=osu1406218333.

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Machado, murtinheiras martins Andre. "Statistical analysis of large scale surveys for constraining the Galaxy evolution." Thesis, Besançon, 2014. http://www.theses.fr/2014BESA2026/document.

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La formation et l'évolution du disque épais de la Voie Lactée restent controversées. Nous avons utilisé un modèle de synthèse de la population de la Galaxie, le Modèle de la Galaxie de Besançon (Robin et al., 2003), qui peut être utilisé pour l'interprétation des données, étudier la structure galactique et tester différents scénarios de formation et évolution Galactique. Nous avons examiné ces questions en étudiant la forme et la distribution de métallicité du disque mince et du disque épais en utilisant l'approche de synthèse de la population. Nous avons imposé sur des simulations les erreurs

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Rafieferantsoa, Mika Harisetry. "The impact of environment and mergers on the H I content of galaxies in hydrodynamic simulations." University of the Western Cape, 2015. http://hdl.handle.net/11394/4763.

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>Magister Scientiae - MSc<br>We quantitatively examine the effects of merger and environment within a cosmological hydrodynamic simulation. We show that our simulation model broadly reproduces the observed scatter in H I at a given stellar mass as quantified by the HI mass function in bins of stellar mass, as well as the H I richness versus local galaxy density. The predicted H I fluctuations and environmental effects are roughly consistent with data, though some discrepancies are present at group scales. For satellite galaxies in & 1012Mhalos, the H I richness distribution is bimodal and drop

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Torrey, Paul A. "Modeling the Evolution of Galaxy Properties across Cosmic Time with Numerical Simulations." Thesis, Harvard University, 2014. http://dissertations.umi.com/gsas.harvard:11496.

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We present a series of numerical galaxy formation studies which apply new numerical methods to produce increasingly realistic galaxy formation models. We first investigate the metallicity evolution of a large set of idealized hydrodynamical galaxy merger simulations of colliding galaxies. We find that inflows of metal--poor interstellar gas triggered by galaxy tidal interactions can account for the systematically lower central oxygen abundances observed in local interacting galaxies. We show the central metallicity evolution during merger events is determined by a competition between the in

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46

Snyder, Gregory Frantz. "Modeling Spatially and Spectrally Resolved Observations to Diagnose the Formation of Elliptical Galaxies." Thesis, Harvard University, 2013. http://dissertations.umi.com/gsas.harvard:10893.

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In extragalactic astronomy, a central challenge is that we cannot directly watch what happens to galaxies before and after they are observed. This dissertation focuses on linking predictions of galaxy time-evolution directly with observations, evaluating how interactions, mergers, and other processes affect the appearance of elliptical galaxies. The primary approach is to combine hydrodynamical simulations of galaxy formation, including all major components, with dust radiative transfer to predict their observational signatures. The current paradigm implies that a quiescent elliptical emerges

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47

Ricciardelli, Elena. "Semi-analytical models of galaxy formation and comparison with observations." Doctoral thesis, Università degli studi di Padova, 2008. http://hdl.handle.net/11577/3426002.

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In this Thesis we attempted to answer to some of the fundamental questions concerning galaxy evolution. In particular when and how galaxies got their present-day stellar content and how this process depends on their mass. In order to address this key issues, we developed a new semi-analytic model of galaxy formation (GECO, Galaxy Evolution COde), that couples a Monte Carlo representation of the hierarchical clustering of dark matter haloes with analytic recipes for the baryonic physics, such as the cooling of the gas, the star formation, the feedback from SN and AGN. We set the model on o

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Finlator, Kristian Markwart. "Comparing Cosmological Hydrodynamic Simulations with Observations of High-Redshift Galaxy Formation." Diss., The University of Arizona, 2009. http://hdl.handle.net/10150/195788.

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We use cosmological hydrodynamic simulations to study the impact of out-flows and radiative feedback on high-redshift galaxies. For outflows, we consider simulations that assume (i) no winds, (ii) a .constant-wind. model in which the mass-loading factor and outflow speed are constant, and (iii) "momentum driven" winds in which both parameters vary smoothly with mass. In order to treat radiative feedback, we develop a moment-based radiative transfer technique that operates in both post-processing and coupled radiative hydrodynamic modes. We first ask how outflows impact the broadband spectral e

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Kriwattanawong, Wichean. "The formation and evolution of the galaxy population in the nearby cluster abell 1367." Thesis, Liverpool John Moores University, 2008. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.502762.

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Valle, Bertoni Luciano Noe del. "Gap formation and its consecuence in the evolution of SMBHS binaries in galaxy mergers." Tesis, Universidad de Chile, 2015. http://repositorio.uchile.cl/handle/2250/136662.

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Doctor en Ciencias, Mención Astronomía<br>En el contexto del modelo de formacion jerárquico, las galaxias son esculpidas por una secuencia de colisiones y eventos de acreción. En algunas de estas colisiones los núcleos de cada galaxia migran a la región central del nuevo sistema y se fusionan, forman- do un nuevo núcleo virializado. Dentro de este nuevo núcleo los agujeros negros super masivos (SMBHs) de cada galaxia migran hacia el centro debido a la fricción dinámi- ca, formando un sistema binario de SMBHs. Entender la evolución de estas binarias es crucial ya que si la separacion de l

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