Thesis (Ph. D.)--University of Texas at Austin, 1998. / Vita. Includes bibliographical references (leaves 124-131). Available also in a digital version from Dissertation Abstracts.

Thesis (Ph. D.)--Montana State University--Bozeman, 2005. / Typescript. Chairperson, Graduate Committee: Sachiko Tsuruta. Includes bibliographical references (leaves 210-219).

Thesis (Ph. D.)--University of Chicago, Dept. of Physics, August 2002. / Includes bibliographical references (p. 31). Also available on the Internet.

Thesis (Ph. D.)--Ohio State University, 2007. / Title from first page of PDF file. Includes bibliographical references (p. 346-357).

In this thesis I discuss probes of small spatial scales around young stars and protostars and around the supermassive black hole at the galactic center. I begin by describing adaptive optics-fed infrared spectroscopic studies of nascent and newborn binary systems. Binary star formation is a significant mode of star formation that could be responsible for the production of a majority of the galactic stellar population. Better characterization of the binary formation mechanism is important for better understanding many facets of astronomy, from proper estimates of the content of unresolved populations, to stellar evolution and feedback, to planet formation. My work revealed episodic accretion onto the more massive component of the pre-main sequence binary system UY Aur. I also showed changes in the accretion onto the less massive component, revealing contradictory indications of the change in accretion rate when considering disk-based and shock-based tracers. I suggested two scenarios to explain the inconsistency. First, increased accretion should alter the disk structure, puffing it up. This change could obscure the accretion shock onto the central star if the disk is highly inclined. Second, if accretion through the disk is impeded before it makes it all the way onto the central star, then increased disk tracers of accretion would not be accompanied by increased shock tracers. In this case mass must be piling up at some radius in the disk, possibly supplying the material for planet formation or a future burst of accretion. My next project focused on characterizing the atmospheres of very low-mass companions to nearby young stars. Whether these objects form in an extension of the binary-star formation mechanism to very low masses or they form via a different process is an open question. Different accretion histories should result in different atmospheric composition, which can be constrained with spectroscopy. I showed that 3-4 μm spectra of a sample of these objects with effective temperatures greater than 1500 K are similar to the spectra of older more massive brown dwarfs at the same temperature, in contrast to objects at 1000 K that exhibit distinct L-band SEDs. The oldest object in my sample of young companions, 50 My old CD-35 2722 B, appears redder than field dwarfs with similar spectral type based on 1-2.5 μm spectra. This could indicate reduced cloud opacity compared to field dwarfs at the same temperature. I also present work to better understand the supermassive blackhole at the center of our Galaxy. Astrometric monitoring of stellar orbits about the blackhole have been used to sketch the gravitational potential, revealing 4 x 10⁶ M_⊙ within a radius of 40 AU. Further constraints on the gravitational potential, and the detection of post-Newtonian effects on the stellar orbits, will require improved astrometric precision. Currently confusion noise in the crowded central cluster limits astrometric precision. Increased spatial resolution can alleviate confusion noise. Dual field phase referencing on large-aperture infrared interferometers provides the sensitivity needed to observe the Galactic center, providing the fastest route to increased spatial resolution. I present simulations of dual-field phase referencing performance with the Keck Interferometer and with the VLTI GRAVITY instrument, to describe the potential contributions each could make to Galactic center stellar astrometry. I demonstrate that the near-future GRAVITY instrument at the VLTI will have a large impact on the ability to precisely track the paths of stars orbiting there, as long as a star with K-band apparent magnitude less than 20 exists within 70 milliarcseconds of the blackhole. Many of the stars orbiting the blackhole are in a post-main sequence wind phase. The wind from these stars is feeding an accretion flow falling onto the blackhole. This flow is radiatively inefficient, producing only 10⁻⁸ times the Eddington limit. Thus our relative proximity to the center of our own Galaxy, provides the opportunity to study a low-luminosity accretion mode that would be difficult or impossible to observe in more remote galaxies. Variable emission from the accretion flow arises from very deep within the flow and could be used to reveal the physics of the accretion process. Characterizing the variability is challenging because all wavelength regimes from radio through X-ray are affected by the process(es) that gives rise to the variations. I report observations of variability at wavelengths that are difficult or challenging to observe from the ground using the SPIRE instrument onboard the Herschel Space Observatory. My work provides the first constraints on the flux of the accretion flow at 250 μm. Variations at 500, 350, and 250 μm observed with Herschel exhibit typical amplitudes similar to the variations observed at 1300 μm from the ground, but the amplitude distribution of flux variations observe with Herschel does not exhibit a tail to large amplitudes that is seen at 1300 μm. This could suggest a connection between large-amplitude mm/submillimeter variations and X-ray activity, since no increased X-ray activity was observed during our Herschel monitoring.

Submitted by Prieslei E. D. Goulart Santos (prieslei@ift.unesp.br) on 2017-12-07T16:59:31Z No. of bitstreams: 1 Thesis.pdf: 1801229 bytes, checksum: 71a64454056164c79eed45a9201789ac (MD5) / Submitted by Prieslei E. D. Goulart Santos (prieslei@ift.unesp.br) on 2017-12-11T18:47:11Z No. of bitstreams: 1 Thesis.pdf: 1801229 bytes, checksum: 71a64454056164c79eed45a9201789ac (MD5) / Submitted by Prieslei E. D. Goulart Santos (prieslei@ift.unesp.br) on 2017-12-14T11:25:03Z No. of bitstreams: 1 Thesis.pdf: 1801229 bytes, checksum: 71a64454056164c79eed45a9201789ac (MD5) / Submitted by Prieslei E. D. Goulart Santos (prieslei@ift.unesp.br) on 2017-12-14T13:50:32Z No. of bitstreams: 1 Thesis.pdf: 1801229 bytes, checksum: 71a64454056164c79eed45a9201789ac (MD5) / Approved for entry into archive by Hellen Sayuri Sato null (hellen@ift.unesp.br) on 2017-12-15T16:09:41Z (GMT) No. of bitstreams: 1 goulartsantos_ped_dr_ift.pdf: 1801229 bytes, checksum: 71a64454056164c79eed45a9201789ac (MD5) / Made available in DSpace on 2017-12-15T16:09:41Z (GMT). No. of bitstreams: 1 goulartsantos_ped_dr_ift.pdf: 1801229 bytes, checksum: 71a64454056164c79eed45a9201789ac (MD5) Previous issue date: 2017-11-21 / Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP) / No contexto de teorias de Einstein-Maxwell-dilaton, estudamos buracos negros, buracos de minhoca e aplicações à correspondência anti-de Sitter/Teoria de Matéria Condensada. Apresentamos a solução de buracos negro dyonica para a teoria de Einstein-Maxwell-dilaton escrita completamente em termos de constantes de integração, e então investigamos como definir parâmetros físicos dependentes e independentes. Escolhendo condições de contorno apropriadas para o dilaton no infinito, construímos buracos negros sem massa e uma ponte de Einstein-Rosen que satisfaz a condição de energia nula. Construímos uma solução carregada analítica de buraco de minhoca atravessável para a teoria de Einstein-Maxwell-phantom-dilaton que é livre de singularidades e conecta dois espaços de Minkowski. Usando o teorema de Gauss-Bonnet calculamos o ângulo de deflexão de um raio de luz que passa próximo este buraco de minhoca. Apresentamos o formalismo da função entropia de Sen e o aplicamos para o cálculo analítico da entropia do buraco negro extremo de uma teoria de supergravidade com N=8 em quatro dimensões. No contexto de holografia, calculamos coeficientes de transporte na presença de campos magnéticos para teorias com um termo topológico na ação. Definimos quantidades radialmente independentes subtraindo as correntes de magnetização, e então estudamos perturbações lineares em torno do horizonte a fim de expressar as condutividades elétrica, termoelétrica e térmica em termos de somente propriedades do horizonte. Combinamos as fórmulas para as condutividades com os dados do horizonte calculados usando o formalismo de Sen, e expressamos analiticamente as condutividades à temperatura zero para várias teorias cujas soluções de buraco negro não são conhecidas analiticamente. / In the context of Einstein-Maxwell-dilaton theory, we study black holes, wormholes and applications to the anti-de Sitter/Condensed Matter Theory correspondence. We present the dyonic black hole solution to the Einstein-Maxwell-dilaton theory written fully in terms of integration constants, and then investigate how to define dependent and independent physical parameters. Choosing appropriate boundary conditions for the dilaton at infinity, we construct massless black holes and an Einstein-Rosen bridge that satisfies the null energy condition. We construct an analytical charged traversable wormhole solution to the Einstein-Maxwell-phantom-dilaton theory which is free of singularities and connects two Minkowski spacetimes. Using the Gauss-Bonnet theorem we compute the deflection angle of a light ray passing close to this wormhole. We present the Sen's entropy function method and apply it to compute analytically the entropy of the extremal black hole of a gauged N=8 supergravity theory in four dimensions. In the holographic context, we compute the transport coefficients in the presence of magnetic fields for theories with a topological term in the action. We define radially independent quantities by subtracting off the magnetization currents, and then study linear perturbations around the horizon in order to express the electric, thermoelectric and heat conductivities in terms of horizon properties only. We combine the formulae for the conductivities with the horizon data computed using Sen's entropy function method, and express analytically the conductivities at zero temperature for several theories whose the full black hole solutions are not known analytically. / 2103/00140-7

No description available.

This thesis considers various topics and open questions in galaxy formation during the epoch of reionization and presents multiple new computational techniques developed specifically to study this era. This work naturally divides into two main sections: 1) The formation of the first massive black holes and 2) Interpreting ALMA observations of galaxy formation during the epoch of reionization. The first topic addresses the existence of super massive black holes (SMBHs) with $M_{\rm BH} > 10^9$M$_{\odot}$ at $z > 6$. It is well established that stellar mass black holes are very unlikely to be able to accrete matter efficiently enough to grow to this mass at this redshift. For this reason, many alternative channels have been proposed for black hole formation that produce objects with significantly larger initial masses. In this thesis, I consider a mechanism whereby runaway stellar collisions in dense primordial star clusters form a very massive star that is likely to collapse to an intermediate mass black hole (IMBH) with $M_{\rm BH} > 10^3$M$_{\odot}$. In order to test this scenario, I added 12 species non-equilibrium chemistry to the massively parallel adaptive mesh refinement code RAMSES, and simulated, at sub-pc resolution, the collapse of the first metal-enriched halo which is likely to host a Population II star cluster. The properties of the central gas cloud in the collapsing halo were then extracted from the simulation and used to create initial conditions for the direct N-body integrator, NBODY6. These star clusters were simulated for 3.5Myr (until the first supernova is expected to occur) and it was determined that the properties of the gas clouds that form in cosmological simulations were indeed suitable to form a very massive star by collisional runaway. This suggests that this mechanism is a promising channel for forming the seeds of SMBHs at high redshift. The second topic of this thesis aims to help interpret the plethora of recent and upcoming ALMA observations of star forming galaxies during the epoch of reionization. These observations target far-infrared lines such as [CII] and [OIII] which directly probe the interstellar medium (ISM) of these $z > 6$ galaxies. In order to study this epoch, I employ the RAMSES-RT code, which allows for the computation of multifrequency radiative transfer on-the-fly. I modified this code in a number of ways so that it can handle radiation-coupled H$_2$ non-equilibrium chemistry (including Lyman-Werner band radiation) and I developed the variable speed of light approximation which changes the speed of light in the simulation depending on the density of gas so that ionisation fronts propagate at the correct speed in all gas phases. Cosmological boxes were initialised to include galaxies with masses comparable to the observations of Maiolino et al. (2015) and run at various resolutions to test convergence properties. One of the major goals of this study was to identify the physical mechanism responsible for the spatial offset observed between [CII] and UV/Lyα in many high-redshift galaxies.

The study of general relativity in higher dimensions has proven to be a fruitful avenue of research, revealing new applications of the theory, for instance in understanding strongly coupled quantum field theories through the holographic principle, and proposing an explanation of the hierarchy problem through TeV gravity scenarios. To understand the non-linear regime of higher dimensional general relativity, such as that involved in the merger of black holes, we use numerical relativity to solve the Einstein equations. In this thesis we develop and demonstrate several diagnostic tools and new initial data for use in numerical relativity simulations of higher dimensional spacetimes, and use these to investigate binary black hole systems. Firstly, we present a formalism for calculating the gravitational waves in a numerical simulation of a higher dimensional spacetime, and apply this formalism to the example of the head on merger of two equal mass black holes. In doing so, we simulate the merger of black holes in up to 10 spacetime dimensions for the first time, and investigate the dependence of the energy radiated away in gravitational waves on the number of dimensions. We also apply this formalism to the example of head on unequal mass black hole collisions, investigating the dependence of radiated energy and momentum on the number of dimensions and the mass ratio. This study complements and sheds further light on previous work on the merger of point particles with black holes in higher dimensions, and presents evidence for a link between the regime studied, and the large $D$ regime of general relativity where $D$ is the number of spacetime dimensions. We also present initial data that enables us to study black holes with initial momentum and angular momentum, putting in place the framework needed to study problems such as the scattering cross section of black holes in higher dimensions, and the nature of black hole orbits in higher dimensions. Finally, we present, and demonstrate the use of, an apparent horizon finder for higher dimensional spacetimes. This allows us to calculate a black hole's mass and spin, which characterise the black hole.

A finalidade deste trabalho é estabelecer as conexões entre física de buracos negros e termodinâmica, atentando para eventuais semelhanças e diferenças entre ramos aparentemente bem diversos da física moderna. Tais conexões foram inicialmente buscadas e estabelecidas na década de 1970, graças ao trabalho de S. Hawking e Jacob D. Bekenstein, entre outros, e sucessivamente aprofundadas nos anos subseqüentes, notadamente na última década. O mérito maior do primeiro foi estabelecer a emissão de radiação com espectro térmico por buracos negros em geral, mesmo aqueles desprovidos de rotação e carga (buracos negros de Schwarzschild). O segundo encarregou-se de correlacionar leis termodinâmicas clássicas com processos envolvendo buracos negros. Neste trabalho, procuramos inicialmente estudar os buracos negros de Schwarzschild e Kerr-Newman no tocante às suas propriedades gerais, bem como o problema do movimento de partículas nos espaços-tempos em questão, para discutir-se brevemente o problema de extração de energia de buracos negros, como apontado por Penrose e outros. Estabelecidas as propriedades gerais, pode-se enfim derivar a Termodinâmica destes buracos, correlacionando-se entropia e área, e obter expressões para a temperatura de corpo negro dos mesmos - em perfeita consonância com a derivação de Hawking, não abordada aqui, feita através da Teoria Quântica de Campos. Com a temperatura, pode-se estudar as capacidades térmicas, reveladores de propriedades típicas de buracos negros não compartilhadas por sistemas clássicos. A reboque destas, entra a discussão sobre a estabilidade termodinâmica de buracos negros em ensembles canônicos e microcanônicos, através do método das séries lineares, de Poincaré, fechando o presente trabalho. Assim, os capítulos 1 e 2 tratam das soluções de Schwarzschild e Kerr-Newman, respectivamente, abordando-lhes as propriedades gerais e o problema do movimento de partículas, materiais ou não, nessas geometrias. O capítulo 3 estabelece as pontes entre Termodinâmica e buracos negros, sendo crucial para o restante do trabalho. No capítulo 4 estudamos temperaturas e capacidades térmicas de diversos buracos negros, e finalmente no capítulo 5 vem o problema da estabilidade termodinâmica dos buracos negros. / In the present work, we have established the connections between black-hole physics and thermodynamics, searching for similarities and differences between these two branches of physicxs, which might look quite far apart. Such links were first sought for and established during the 1970s, thanks to the pioneering work of S. Hawking and Jacob D. Bekenstein, among others, and continuously developed in the following years, notably in the last decade. Hawking's major achievement was the prediction, from arguments based on Quantum Field Theory, that black holes radiate with a thermal spectrum, even the uncharged and nonrotating ones (the Schwarzschild black holes). Bekenstein's biggest merit was to find the link between classical thermodynamical laws and processes involving black holes. In this work, we started with Schwarzschild and Kerr-Newman black holes, working out their general properties, as well as the problem of particle motion in such spacetimes, so that we could briefly discuss the issue of energy extraction from black holes, as established by Penrose and others. Once the general features of these black holes were known, it was possible to derive the black-hole thermodynamics, due to a simple relation between black-hole entropy and area. Expressions for the black-hole temperature were then easily obtained, in perfect agreement with Hawking's own derivation, not considered here. With temperatures at hand, heat capacities could be thoroughly examined, showing intrinsic properties of black holes, not shared by classical systems. The question of thermodynamic stability of black holes arose naturally from heat capacity analysis, and we have analysed black holes in both the microcanonical and canonical ensembles, in the light of Poincaré's linear series method, completing the current work. Chapters 1 and 2 deal with the Schwarzschild and Kerr-Newman solutions, respectively, deriving their general features and working out particle motion in these geometries. Chapter 3 establishes the links between black-hole physics and thermodynamics, being of crucial importance for the subsequent chapters. Chapter 4 provides an extensive study of black-hole temperatures and heat capacities, paving the way for the last chapter, Chapter 5, concerning to thermodynamic stability of black holes.