O plasma de quarks e gluons (QGP) em temperatura zero e alta densidade bariônica é um sistema que pode existir no interior de estrelas densas. É possível que esse QGP frio compartilhe algumas características com o plasma quente, observado em colisões de íons pesados relativísticos, sendo também um sistema fortemente interagente. Neste trabalho, utilizamos uma equação de estado derivada a partir da QCD e a aplicamos no estudo de estrutura estelar. Mostramos que nossos resultados são compatíveis com o pulsar PSR J1614 2230 de massa (1.97 ± 0.04)M. / The Quark Gluon Plasma (QGP) at zero temperature and high baryon number is a system that may exist in the core of dense stars. This cold QGP has a rich phase structure and at high enough chemical potential it is quite possible that it shares some features with the hot QGP observed in heavy ion collisions, being also a strongly interacting system. We use an equation of state derived from QCD and apply it to study of stellar structure. Our results reproduce the measured mass, (1.97 ± 0.04)M, of the pulsar PSR J1614 2230.

Exact solutions to Einstein's field equations in the presence of matter are presented. A one parameter family of interior solutions for a static fluid is discussed. It is shown that these solutions can be joined to the Schwarzschild exterior, and hence represent fluid spheres of finite radius. Contained within this family is a set of solutions which are gaseous spheres defined by the vanishing of the density at the surface. One such solution yields an analytic expression which corresponds to the asymptotic numerical solution of Oppenheimer and Volkoff for the degenerate neutron gas. These gaseous spheres have ratios of specific heats that lie between one and two in the vicinity of the origin, increasing outward, but remaining less than the velocity of light throughout.

O plasma de quarks e gluons (QGP) em temperatura zero e alta densidade bariônica é um sistema que pode existir no interior de estrelas densas. É possível que esse QGP frio compartilhe algumas características com o plasma quente, observado em colisões de íons pesados relativísticos, sendo também um sistema fortemente interagente. Neste trabalho, utilizamos uma equação de estado derivada a partir da QCD e a aplicamos no estudo de estrutura estelar. Mostramos que nossos resultados são compatíveis com o pulsar PSR J1614 2230 de massa (1.97 ± 0.04)M. / The Quark Gluon Plasma (QGP) at zero temperature and high baryon number is a system that may exist in the core of dense stars. This cold QGP has a rich phase structure and at high enough chemical potential it is quite possible that it shares some features with the hot QGP observed in heavy ion collisions, being also a strongly interacting system. We use an equation of state derived from QCD and apply it to study of stellar structure. Our results reproduce the measured mass, (1.97 ± 0.04)M, of the pulsar PSR J1614 2230.

published_or_final_version / Physics / Doctoral / Doctor of Philosophy

<p>Neutron stars are some of the most fascinating objects in Nature. Essentially all aspects of physics seems to be represented inside them. Their cores are likely to contain deconfined quarks, hyperons and other exotic phases of matter in which the strong interaction is the dominant force. The inner region of their solid crust is penetrated by superfluid neutrons and their magnetic fields may reach well over 10¹²Gauss. Moreover, their extreme mean densities, well above the densities of nuclei, and their rapid rotation rates makes them truly relativistic both in the special as well as in the general sense. This thesis deals with a small subset of these phenomena. In particular the exciting possibility of trapping of gravita-tional waves is examined from a theoretical point of view. It is shown that the standard condition <i>R</i> < 3<i>M</i> is not essential to the trapping mechanism. This point is illustrated using the elegant tool provided by the optical geometry. It is also shown that a realistic equation of state proposed in the literature allows stable neutron star models with closed circular null orbits, something which is closely related to trapped gravitational waves. Furthermore, the general relativistic theory of elasticity is reviewed and applied to stellar models. Both static equilibrium as well as radially oscillating configurations with elasticsources are examined. Finally, Killing tensors are considered and their applicability to modeling of stars is discussed</p>

Neutron stars are amongst the most exotic objects known in the universe; more than a solar mass of material is squeezed into an object the size of a city, leading to a density comparable to that of an atomic nucleus. They have a surface magnetic field which is typically around a trillion times stronger than the magnetic field here on Earth, and we have observed them to spin up to around 700 times per second. The existence of neutron stars was first proposed by Baade and Zwicky in 1934 but later graduated from theory to fact in 1967 as the first pulses were detected by Jocelyn Bell-Burnell, a then graduate student at the University of Cambridge. There are now well over 2000 neutron stars whose radio emission beams point at, and have been detected on Earth. We call these objects pulsars. Because of their remarkable properties, pulsars are very useful to physicists, who can employ them as precision timing tools due to the unwavering nature of their emission and of their rotation. Having an array of ultra-accurate clocks scattered throughout our galaxy is very useful for performing astrophysical experiments. In particular, precise pulsar timing measurements and the models that explain them, will permit the direct detection of gravitational radiation; a stochastic background initially, and potentially the individual signals from supermassive black hole binaries. Our models of pulsar behaviour are so precise that we are now able to notice even slight departures from them; we are starting to see that unmodelled variability in pulsars occurs over a broad range of timescales, both in emission and in rotation. Any unmodelled variability is, of course, detrimental to the pulsar's utility as a precision timing tool, and presents a problem when looking for the faint effects of a passing gravitational wave. We are hoping that pulsar timing arrays will detect gravitational radiation in the coming decade, but this depends, in part, on our ability to understand and mitigate the effects of the unmodelled intrinsic instabilities that we are observing. One important clue as to the nature of the variability in pulsar emission and rotation, is the emerging relationship between the two; we sometimes observe correlation on timescales of months and years. We have been observing pulsars for almost fifty years and our expanding datasets now document decades of pulsar behaviour. This gives us the ability to investigate pulsar variability on a range of timescales and to gain an insight into the physical processes that govern these enigmatic objects. In this thesis I describe new techniques to detect and analyse the emission and rotational variability of radio pulsars. We have employed these techniques on a 24 year pulsar dataset to unearth a striking new example of a dramatic and simultaneous shift in a pulsar's emission and rotation. We hypothesise that this event was caused by an asteroid interaction, although other explanations are also possible. Our variability techniques have also been used to analyse data from 168 young, energetic pulsars. In this thesis we present results from the nine most interesting. Of these, we have found some level of correlated variability in seven, one of which displays it very strongly. We have also assessed the emission stability of the NANOGrav millisecond pulsars and have found differing degrees of variability, due to both instrumental and astrophysical causes. Finally, we propose a method of probing the relationship between emission and rotation on short-timescales and, using a simulation, we have shown the conditions under which this is possible. Throughout the work, we address the variability in pulsar emission, rotation and links between the two, with the aim of improving pulsar timing, attaining a consolidated understanding of the diverse variable phenomena observed and elucidating the evolutionary path taken by pulsars.

Orientadores: Cecilia Bertoni Martha Hadler Chirenti, Ernesto Kemp / Tese (doutorado) - Universidade Estadual de Campinas, Instituto de Física Gleb Wataghin / Made available in DSpace on 2018-09-03T00:23:17Z (GMT). No. of bitstreams: 1 Souza_GibranHenriqueDe_D.pdf: 9537099 bytes, checksum: 8b4790f32975067863cff845c7c37170 (MD5) Previous issue date: 2017 / Resumo: No presente trabalho focamos na descrição das oscilações da crosta de estrelas de nêutrons que apresentam um campo magnético poloidal com uma componente toroidal, onde utilizamos de oito equações de estado para descrever a matéria constituinte destas estrelas de nêutrons. Para isso apresentamos todo o formalismo matemático para descrever a estrutura interna, rotação, campo magnético e perturbações no fluido necessário para a apresentação dos resultados obtidos. Paralelo a isso efetuamos a extensão dos resultados obtidos na dissertação de mestrado, onde foi apresentado o cálculo das características das ondas gravitacionais do modo-f, como frequência de oscilação e tempo de decaimento. Aqui estendemos os resultados anteriormente obtidos com a inclusão de novas equações de estado e o teste da validade das chamadas relações universais / Abstract: In the present work we focus on the description of the crustal oscillations of neutron stars that present a poloidal magnetic field with a toroidal component, where we use eight equations of state to describe the constituent matter of these neutron stars. For this, we developed all the mathematical formalism to describe the internal structure, rotation, magnetic field and perturbations in the fluid necessary for the presentation of the obtained results. Parallel to this, we extended the results obtained in the student's master dissertation, where the calculation of the characteristics of the f-mode gravitational waves was presented, such as oscillation frequency and decay time. Here we extend the previously obtained results with the inclusion of new state equations and the test of the validity of the so-called universal relations / Doutorado / Física / Doutor em Ciências / 140838/2013-9 / CNPQ

Ho, Tak Ngai = 中子星在絶熱冷卻下的不穩定性 : 數值模擬和簡單類比 / 何德藝. / Thesis (M.Phil.)--Chinese University of Hong Kong, 2011. / Includes bibliographical references (leaves 101-102). / Abstracts in English and Chinese. / Ho, Tak Ngai = Zhong zi xing zai jue re leng que xia de bu wen ding xing : shu zhi mo ni he jian dan lei bi / He Deyi. / Chapter 1 --- Introduction --- p.1 / Chapter 2 --- The astrophysical problem --- p.2 / Chapter 2.1 --- Neutron stars --- p.2 / Chapter 2.2 --- Equations --- p.4 / Chapter 2.3 --- EOS --- p.6 / Chapter 2.4 --- Equilibrium configurations --- p.8 / Chapter 2.5 --- Stability --- p.9 / Chapter 2.6 --- The key equilibrium properties --- p.10 / Chapter 2.7 --- Adiabatic cooling --- p.11 / Chapter 2.8 --- Modeling adiabatic cooling by varying T --- p.13 / Chapter 3 --- Numerical Simulations in GR --- p.17 / Chapter 3.1 --- Introduction --- p.17 / Chapter 3.2 --- The equations and the EOS --- p.17 / Chapter 3.3 --- Evolution of a stellar system in GR --- p.20 / Chapter 3.4 --- Results --- p.22 / Chapter 4 --- Newtonian model --- p.27 / Chapter 4.1 --- Introduction --- p.27 / Chapter 4.2 --- Newtonian fluid equations --- p.28 / Chapter 4.3 --- Polytropes --- p.28 / Chapter 4.4 --- Model EOS --- p.31 / Chapter 4.5 --- Equilibrium solutions --- p.33 / Chapter 4.6 --- Stability --- p.35 / Chapter 4.7 --- Dynamics --- p.38 / Chapter 4.8 --- Adiabatic changes --- p.42 / Chapter 4.9 --- Results --- p.46 / Chapter 5 --- Model of instability --- p.52 / Chapter 5.1 --- Introduction . --- p.52 / Chapter 5.2 --- Analytical study of the model --- p.54 / Chapter 5.3 --- Numerical verification --- p.55 / Chapter 5.4 --- Summary --- p.59 / Chapter 6 --- Model of criticality --- p.62 / Chapter 6.1 --- Introduction --- p.62 / Chapter 6.2 --- General discussion of equilibrium properties --- p.63 / Chapter 6.3 --- Construction of model --- p.67 / Chapter 6.4 --- Study of the model --- p.75 / Chapter 6.5 --- Conclusion --- p.82 / Chapter 7 --- Conclusion --- p.85 / Appendix --- p.87 / Chapter A --- Neutron stars cooling due to neutrinos emission --- p.87 / Chapter B --- Determining how r change --- p.89 / Chapter C --- Basic equations in the GR context --- p.91 / Chapter C.1 --- ADM formulation of the field equations --- p.91 / Chapter C.2 --- Explicit form of the hyperbolic equation --- p.93 / Chapter D --- One-zone model --- p.95 / Chapter E --- Numerical scheme of getting the EOS --- p.98 / Bibliography --- p.101

Zhang, Yaojun = / "November 2009." / Thesis (M.Phil.)--Chinese University of Hong Kong, 2010. / Includes bibliographical references (p. 109-111). / Abstracts in English and Chinese. / Zhang, Yaojun = / Abstract --- p.i / Acknowledgement --- p.iv / Chapter 1 --- Introduction --- p.1 / Chapter 2 --- Quasi-Normal Modes of Neutron Stars --- p.6 / Chapter 2.1 --- Equilibrium State of a Neutron Star --- p.6 / Chapter 2.2 --- Fluid Displacement and Metric Perturbation --- p.8 / Chapter 2.3 --- Axial Oscillations of Neutron Stars --- p.9 / Chapter 2.3.1 --- Wave Equation inside the Star --- p.9 / Chapter 2.3.2 --- Wave Equation outside the Star --- p.10 / Chapter 2.3.3 --- Location of Quasi-normal Modes --- p.10 / Chapter 2.4 --- Polar Oscillations of Neutron Stars - LD Formalism --- p.12 / Chapter 2.4.1 --- Equations inside the Star --- p.12 / Chapter 2.4.2 --- Equations outside the Star --- p.14 / Chapter 2.4.3 --- Location of Quasi-normal Modes --- p.16 / Chapter 2.5 --- Polar Oscillations of Neutron Stars - AAKS Formalism --- p.16 / Chapter 2.5.1 --- Equations inside the Star --- p.16 / Chapter 2.5.2 --- Equations outside the Star --- p.19 / Chapter 2.5.3 --- Location of Quasi-normal Modes --- p.19 / Chapter 3 --- Decoupling of Spacetime Oscillations and Fluid Motion --- p.21 / Chapter 3.1 --- Motivation of Decoupling --- p.21 / Chapter 3.2 --- Expressing F in terms of S and H --- p.21 / Chapter 3.2.1 --- Inside the Star --- p.22 / Chapter 3.2.2 --- Outside the Star --- p.25 / Chapter 3.3 --- Constraint-free AAKS Formalism --- p.25 / Chapter 3.3.1 --- Equations inside the Star --- p.25 / Chapter 3.3.2 --- Equations outside the Star --- p.27 / Chapter 3.4 --- Cowling Approximation for Polar p-Mode --- p.29 / Chapter 3.4.1 --- Independent Fluid Motion --- p.29 / Chapter 3.4.2 --- Location of Polar p-Modes --- p.30 / Chapter 3.4.3 --- Numerical Results and Discussion --- p.31 / Chapter 3.5 --- Inverse-Cowling approximation for ω-Mode --- p.33 / Chapter 3.5.1 --- Independent Spacetime Oscillations --- p.33 / Chapter 3.5.2 --- Location of ω-Modes --- p.34 / Chapter 3.5.3 --- Numerical Results and Discussion --- p.34 / Chapter 4 --- Interplay between Matter and Spacetime --- p.37 / Chapter 4.1 --- Physical Insight --- p.37 / Chapter 4.2 --- Sturm-Liouville Eigenvalue Problem --- p.39 / Chapter 4.3 --- Energy of the Fluid --- p.40 / Chapter 4.4 --- Spacetime Oscillation Driven by Fluid Motion --- p.45 / Chapter 4.5 --- Damped Oscillation Caused by Radiation of Gravitational Wave --- p.46 / Chapter 4.6 --- Calculation of δωn in a Perturbative Way --- p.48 / Chapter 4.7 --- Numerical Results and Discussion --- p.49 / Chapter 5 --- Asymptotic Behavior of Spacetime Modes --- p.61 / Chapter 5.1 --- Motivation --- p.61 / Chapter 5.2 --- Asymptotic Behavior of Axial ω-modes for One-Layered Stars --- p.62 / Chapter 5.2.1 --- "Asymptotic Form of g(r*,ω)" --- p.63 / Chapter 5.2.2 --- "Asymptotic Form of f(r*, ω)" --- p.67 / Chapter 5.2.3 --- Asymptotic Behavior of Axial Quasi-Normal Modes --- p.69 / Chapter 5.3 --- Asymptotic Behavior of Polar ω-modes for One-Layered Stars --- p.71 / Chapter 5.3.1 --- High-Frequency Approximation --- p.71 / Chapter 5.3.2 --- Asymptotic Behavior of Polar Quasi-Normal Modes --- p.73 / Chapter 5.4 --- Relationship between Axial and Polar ω-Modes --- p.74 / Chapter 5.4.1 --- Application 1:ω-Modes of Quark Stars --- p.75 / Chapter 5.4.2 --- Application 2:ω-Modes of Polytropic Stars --- p.80 / Chapter 5.4.3 --- Application 3: The Influence of Surface Discontinuities --- p.89 / Chapter 5.4.4 --- Application 4:ω-Modes of Realistic Neutron Stars --- p.92 / Chapter 6 --- Conclusion and Outlook --- p.99 / Chapter A --- From Einstein Equation to LD Formalism --- p.101 / Chapter A.l --- The Linearized Perturbation Equations --- p.101 / Chapter A.1.1 --- The Perturbation of the Einstein Tensor --- p.102 / Chapter A.1.2 --- The Perturbation of the Energy-momentum Tensor --- p.103 / Chapter A.1.3 --- The Perturbed Einstein Equations --- p.104 / Chapter A.2 --- Some Symbolic Operation Results --- p.105 / Chapter A.3 --- Simplifications --- p.106

This thesis considers the various morphologies of radio supernova remnants (SNRs), and attempts to determine whether their appearance results from the properties of the progenitor star and its supernova explosion, or from the structure of the interstellar medium (ISM) and ambient magnetic field into which a SNR consequently expands. High-resolution observations of Supernova 1987A show a young remnant whose appearance and evolution are completely dominated by the structure of its progenitor wind. A statistical study of the Galactic population of bilateral SNRs demonstrates that the symmetry axes of these remnants run parallel to the Galactic Plane. This result can be explained by the interaction of main sequence stellar wind-bubbles with the ambient magnetic field; expansion of SNRs into the resulting elongated cavities results in a bilateral appearance with the observed alignment. Radio observations of SNR G296.8-00.3 show a double-ringed morphology which is best explained by expansion either into an anisotropic main-sequence progenitor wind or into multiple cavities in the ISM. Data on SNRs G309.2-00.6 and G320.4-01.2 (MSH 15-52) make a strong case that the appearance of both remnants is significantly affected by collimated outflows from a central source; for G309.2-00.6 the source itself is not detected, but for G320.4-01.2 there is now compelling evidence that the remnant is associated with and is interacting with the young pulsar PSR B1509-58. I conclude that, while the youngest SNRs are shaped by their progenitor's circumstellar material, the appearance of most SNRs reflects the properties of the local ISM and magnetic field. Remnants which interact with an associated pulsar or binary system appear to be rare, and are easily distinguished by their unusual and distorted morphologies.