Download or read book Rotating Neutron Stars and the Equation of State of Dense Matter written by and published by . This book was released on 1990 with total page 16 pages. Available in PDF, EPUB and Kindle. Book excerpt: We investigate the properties of non-rotating as well as rotating neutron stars in the framework of Einstein's theory of general relativity. The nuclear equation of state of neutron star matter (electrically charge neutral many-baryon/lepton system) is calculated for the relativistic Hartree- and Hartree-Fock approximations. The influence of two-particle correlations on the equation of state is taken into account, too. An important result is that the limiting rotational frequency of a neutron star is set by instability modes caused by gravitational radiation reaction, which set in well below the Kerplerian frequency. 20 refs., 7 figs., 3 tabs.
Download or read book Neutron Stars 1 written by P. Haensel and published by Springer Science & Business Media. This book was released on 2007-12-06 with total page 633 pages. Available in PDF, EPUB and Kindle. Book excerpt: The book gives an extended review of theoretical and observational aspects of neutron star physics. With masses comparable to that of the Sun and radii of about ten kilometres, neutron stars are the densest stars in the Universe. This book describes all layers of neutron stars, from the surface to the core, with the emphasis on their structure and equation of state. Theories of dense matter are reviewed, and used to construct neutron star models. Hypothetical strange quark stars and possible exotic phases in neutron star cores are also discussed. Also covered are the effects of strong magnetic fields in neutron star envelopes.
Download or read book Neutron Stars Fast Pulsars Supernovae and the Equation of State of Dense Matter written by and published by . This book was released on 1989 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt: We discuss the prospects for obtaining constraints on the equation of state from astrophysical sources. Neutron star masses although few are known at present, provide a very direct constraint in as much as the connection to the equation of state involves only the assumption that Einstein's general theory of relativity is correct at the macroscopic scale. If the millisecond pulses briefly observed in the remnant of SN1987A can be attributed to uniform rotation of a pulsar, then a very severe constraint is placed on the equation of state. The theory again is very secure. The precise nature of the constraint is not yet understood, but it appears that the equation of state must be neither too soft nor stiff, and it may be that there is information not only on the stiffness of the equation of state but on its shape. Supernovae simulations involve such a plethora of physical processes including those involved in the evolution of the precollapse configuration, not all of them known or understood, that they provide no constraint at the present time. Not even the broad category of mechanism for the explosion is agreed upon (prompt shock, delayed shock, or nuclear explosion). In connection with very fast pulsars, we include some speculations on pure quark matter stars, and on possible scenarios for understanding the disappearance of the fast pulsar in SN1987A. 47 refs., 16 figs., 1 tab.
Download or read book The Physics and Astrophysics of Neutron Stars written by Luciano Rezzolla and published by Springer. This book was released on 2019-01-09 with total page 811 pages. Available in PDF, EPUB and Kindle. Book excerpt: This book summarizes the recent progress in the physics and astrophysics of neutron stars and, most importantly, it identifies and develops effective strategies to explore, both theoretically and observationally, the many remaining open questions in the field. Because of its significance in the solution of many fundamental questions in nuclear physics, astrophysics and gravitational physics, the study of neutron stars has seen enormous progress over the last years and has been very successful in improving our understanding in these fascinating compact objects. The book addresses a wide spectrum of readers, from students to senior researchers. Thirteen chapters written by internationally renowned experts offer a thorough overview of the various facets of this interdisciplinary science, from neutron star formation in supernovae, pulsars, equations of state super dense matter, gravitational wave emission, to alternative theories of gravity. The book was initiated by the European Cooperation in Science and Technology (COST) Action MP1304 “Exploring fundamental physics with compact stars” (NewCompStar).
Download or read book Relativistic Hydrodynamics written by Luciano Rezzolla and published by OUP Oxford. This book was released on 2013-09-26 with total page 752 pages. Available in PDF, EPUB and Kindle. Book excerpt: Relativistic hydrodynamics is a very successful theoretical framework to describe the dynamics of matter from scales as small as those of colliding elementary particles, up to the largest scales in the universe. This book provides an up-to-date, lively, and approachable introduction to the mathematical formalism, numerical techniques, and applications of relativistic hydrodynamics. The topic is typically covered either by very formal or by very phenomenological books, but is instead presented here in a form that will be appreciated both by students and researchers in the field. The topics covered in the book are the results of work carried out over the last 40 years, which can be found in rather technical research articles with dissimilar notations and styles. The book is not just a collection of scattered information, but a well-organized description of relativistic hydrodynamics, from the basic principles of statistical kinetic theory, down to the technical aspects of numerical methods devised for the solution of the equations, and over to the applications in modern physics and astrophysics. Numerous figures, diagrams, and a variety of exercises aid the material in the book. The most obvious applications of this work range from astrophysics (black holes, neutron stars, gamma-ray bursts, and active galaxies) to cosmology (early-universe hydrodynamics and phase transitions) and particle physics (heavy-ion collisions). It is often said that fluids are either seen as solutions of partial differential equations or as "wet". Fluids in this book are definitely wet, but the mathematical beauty of differential equations is not washed out.
Download or read book Equation of State of Neutron Star Matter Limiting Rotational Periods of Fast Pulsars and the Properties of Strange Stars written by and published by . This book was released on 1993 with total page 15 pages. Available in PDF, EPUB and Kindle. Book excerpt: In this paper the following items will be treated: The present status of dense nuclear matter calculations and constraints on the behavior of the associated equation of state at high densities from data on rapidly rotating pulsars. Recent finding of the likely existence of a mixed phase of baryons and quarks forming a coulomb lattice in the dense cores of neutron stars. Review of important findings of recently performed calculations of rapidly rotating compact stars. These are constructed in the framework of general relativity theory for a representative collection of realistic nuclear equations of state. Establish the minimum-possible rotational periods of gravitationally bound neutron stars and self-bound strange stars. Its knowledge is of fundamental importance for the decision between pulsars that can be understood as rotating neutron stars and those that cannot (signature of hypothetical self-bound matter of which strange stars are the likely stellar candidates. Investigate the properties of sequences of strange stars. Specifically, we answer the question whether such objects can give rise to the observed phenomena of pulsar glitches, which is at the present time the only astrophysical test of the strange-quark-matter hypothesis.
Download or read book Supernovae Neutron Star Physics and Nucleosynthesis written by Debades Bandyopadhyay and published by Springer Nature. This book was released on 2022-03-28 with total page 221 pages. Available in PDF, EPUB and Kindle. Book excerpt: This book deals with the interdisciplinary areas of nuclear physics, supernovae and neutron star physics. It addresses the physics and astrophysics of the spectacular supernova explosions, starting with the collapse of massive stars and ending with the birth of neutron stars or black holes. Recent progress in the understanding of core collapse supernova (CCSN) and observational aspects of future detections of neutrinos from CCSN explosions are discussed. The other main focus in this text is the novel phases of dense nuclear matter, its compositions and equation of state (EoS) from low to very high baryon density relevant to supernovae and neutron stars. The multi-messenger astrophysics of binary neutron star merger GW170817 and its relation to EoS through tidal deformability are also presented in detail. The synthesis of elements heavier than iron in the supernova and neutron star environment by the rapid (r)-process are treated here with special emphasis on the nucleosynthesis in the ejected material from GW170817. This monograph is written for graduate students and researchers in the field of nuclear astrophysics.
Download or read book The Cooling of Neutron Stars written by Ronny Kjelsberg and published by Lulu.com. This book was released on 2012-06-21 with total page 120 pages. Available in PDF, EPUB and Kindle. Book excerpt: Neutron stars are the densest objects known in our universe that have not collapsed in on themselves to form a singularity (a black hole). Like black holes they are formed when stars run out of nuclear fuel and radiation pressure can no longer withstand the pull of gravitational forces. This book gives you an in-depth look at how the Direct Urca process is a central element in the cooling of neutron stars after their forming, however it also provides brief introductions to neutron star physics in general, the history of neutron star physics, and pulsars - the pulsating stars that form the observational basis for neutron stars. The book also introduces the different relevant models for an equations of state for neutron stars and a chapter on hyperon matter, before it finally goes on to describe the cooling processes of neutron stars, all with the necessary mathemathical framework for an in-depth analysis.
Download or read book On the Ultimate Density of Stable Neutron Stars written by Oliver Quinn Hamil and published by . This book was released on 2012 with total page 46 pages. Available in PDF, EPUB and Kindle. Book excerpt: With central energy densities many times the density of atomic nuclei, and relatively low temperatures, neutron stars may be some of the best objects in nature from which we are able to study the properties of ultra-dense, cold nuclear matter. With advancements in observational astronomy, more high quality observed data is available than ever before. This study aims to establish a phenomenological model of the macroscopic properties of neutron stars which, when compared with observational data, can give some insight into the physics of the ultra-dense nuclear matter thought to exist in the cores of neutron stars, and help to provide a constraint on the poorly understood equation of state thereof. One example of a well documented neutron star is the Demorest pulsar PSR J1614-2230, which has a well measured mass of 1.97 ± 0.04 M [circle dot operator]. Just from this mass measurement, we can set limits on the radius, central energy-density, and rotation for this pulsar. A parameter scan of neutron star properties is important because it allows us to establish limits on the possible exotic physical processes at work in the extreme environments of neutron star cores. Using the methods described in this thesis, it is possible to explore a wide range of possible physical limits to be set when studying the physics of neutron stars. The equation of state of ultra-dense matter is of key importance for determining the properties of neutron stars, however this equation of state is almost completely unknown. To produce the true equation of state for neutron stars constitutes a very complicated, many-body problem consisting of some 1057 particles. In addition, the nature of the matter existing at the core is a mystery. The basic building blocks of the ultra-dense matter are uncertain, and possible first order phase-transitions may exist. There are competing theoretical frameworks ranging from Schroedinger based, classical considerations, to relativistic quantum theory such as Dirac, to relativistic mean-field theory. These challenges have kept the equation of state of ultra-dense matter in neutron star cores from being fully realized thus far. For this reason, we employ a variational ansatz based on the minimal physical assumptions that the matter in the core of neutron stars exhibits microscopic stability, that causality is not violated, and Einstein's theory of general relativity is the correct theory of gravity. From this ansatz, we create a large number of physically allowed equations of state. Since we are not confined by the parameters of any one particular equation of state model, we have the freedom to run a complete parameter scan of allowed neutron star properties. The parameters established in this thesis give a wide range of physical constraints on the macroscopic properties of neutron stars.
Download or read book Neutron Stars and the Determination of the Dense Matter Equation of State written by Sebastien Guillot and published by . This book was released on 2014 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt: "A physical understanding of the behaviour of cold ultra-dense matter -- at and above nuclear density -- can only be achieved by the study of neutron stars. The surface thermal emission from neutron stars in quiescent low-mass X-ray binaries (qLMXBs) inside globular clusters has proven useful for that purpose. These systems rely on the relatively precisely measured distances to globular clusters to produce measurements of the radiation radius of neutron stars R_infinity, the radius as seen from infinite distance. Such measurements can be compared to the Mass-Radius relation resulting from proposed dense matter equations of state. Individually, the R_infinity measurements from qLMXBs do not produce stringent constraints on the dense matter equation of state. However, when several of these qLMXBs spectra are combined in a coherent manner, they can lead to useful constraints on the dense matter equation of state.This work first presents the discovery of a new spectrally identified qLMXB inside a globular cluster, and the spectral analysis of high signal-to-noise ratio data from another qLMXB, leading to a precise R_infinity measurement. Then, spectra from multiple qLMXBs hosted in globular clusters are combined in a simultaneous analysis using a Markov-Chain Monte-Carlo approach, placing new constraints on the dense matter equation of state. This method and the Bayesian approach developed in this analysis permits including all quantifiable sources of uncertainty (e.g., in the distance, the hydrogen column density) to produce the most conservative constraints on the dense matter equation of state. Finally, this Bayesian approach is modified and adapted to quantitatively reject or confirm a selection of proposed equations of state." --
Download or read book Neutron Stars Strange Stars and the Nuclear Equation of State written by and published by . This book was released on 1992 with total page 28 pages. Available in PDF, EPUB and Kindle. Book excerpt: This article consists of three parts. In part one we review the present status of dense nuclear matter calculations, and introduce a representative collection of realistic nuclear equations of state which are derived for different assumptions about the physical behavior of dense matter (baryon population, pion condensation, .possible transition of baryon matter to quark matter). In part two we review recently performed non-rotating and rotating compact star calculations performed for these equations of state. The minimum stable rotational periods of compact stars, whose knowledge is of decisive importance for the interpretation of rapidly rotating pulsars, axe determined. For this purpose two different limits on stable rotation are studied: rotation at the general relativistic Kepler period (below which mass shedding at the star's equator sets in), and, secondly, rotation at the gravitational radiation-reaction instability (at which emission of gravitational waves set in which slows the star down). Part three of this article deals with the properties of hypothetical strange stars. Specifically we investigate the amount of nuclear solid crust that can be carried by a rotating strange star, and answer the question whether such objects can give rise to the observed phenomena of pulsar glitches, which is at the present time the only astrophysical test of the strange-quark-matter hypothesis.
Download or read book Rotating Relativistic Stars written by John L. Friedman and published by Cambridge University Press. This book was released on 2013-02-11 with total page 435 pages. Available in PDF, EPUB and Kindle. Book excerpt: The masses of neutron stars are limited by an instability to gravitational collapse and an instability driven by gravitational waves limits their spin. Their oscillations are relevant to x-ray observations of accreting binaries and to gravitational wave observations of neutron stars formed during the coalescence of double neutron-star systems. This volume includes more than forty years of research to provide graduate students and researchers in astrophysics, gravitational physics and astronomy with the first self-contained treatment of the structure, stability and oscillations of rotating neutron stars. This monograph treats the equations of stellar equilibrium; key approximations, including slow rotation and perturbations of spherical and rotating stars; stability theory and its applications, from convective stability to the r-mode instability; and numerical methods for computing equilibrium configurations and the nonlinear evolution of their oscillations. The presentation of fundamental equations, results and applications is accessible to readers who do not need the detailed derivations.
Download or read book Saturation of the f mode Instability in Neutron Stars written by Pantelis Pnigouras and published by Springer. This book was released on 2018-09-25 with total page 220 pages. Available in PDF, EPUB and Kindle. Book excerpt: This book presents a study of the saturation of unstable f-modes (fundamental modes) due to low-order nonlinear mode coupling. Since their theoretical prediction in 1934, neutron stars have remained among the most challenging objects in the Universe. Gravitational waves emitted by unstable neutron star oscillations can be used to obtain information about their inner structure, that is, the equation of state of dense nuclear matter. After its initial growth phase, the instability is expected to saturate due to nonlinear effects. The saturation amplitude of the unstable mode determines the detectability of the generated gravitational-wave signal, but also affects the evolution of the neutron star. The study shows that the unstable (parent) mode resonantly couples to pairs of stable (daughter) modes, which drain the parent’s energy and make it saturate via a mechanism called parametric resonance instability. Further, it calculates the saturation amplitude of the most unstable f-mode multipoles throughout their so-called instability windows.
Download or read book Neutron Stars written by Hiroshi Uechi and published by Nova Science Publishers. This book was released on 2012 with total page 0 pages. Available in PDF, EPUB and Kindle. Book excerpt: This book illustrates observed values and properties of neutron stars, field theoretical approaches of hadrons to high density matter, such as nuclear and hyperonic matter, signals of dynamical phenomena, hadronic and hadron-quark neutron stars, radiations from high density matter and supernova phenomena. However, it is not intended to report facts and results at front-line research fields, because numerous conference reports suffice the objectives. The purpose of editing the book is to review related areas of nuclear physics and astrophysics in terms of equations of state of high density matter so as to promote mutual understandings and their consistent progresses. It is focused on theoretical relations between equations of state (EOS) and observables. These topics of high density matter, which extend across many fields of physics, should be frequently reviewed for researchers and people in general.
Download or read book Three Hundred Years of Gravitation written by Stephen Hawking and published by Cambridge University Press. This book was released on 1987 with total page 712 pages. Available in PDF, EPUB and Kindle. Book excerpt: A collection of reviews by prominent researchers in cosmology, relativity and particle physics commemorates the 300th anniversary of Newton's Philosophiae Naturalis Principia Mathematica.
Download or read book Physics of Dense Matter Neutron Stars and Supernova written by and published by . This book was released on 1989 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt: Nuclear and astrophysical evidence on the equation of state of dense matter is examined. The role of hyperonization of matter in the development of proto-neutron stars is briefly discussed. 7 refs., 4 figs.
Download or read book Properties of Massive Neutron Stars written by Susan Elizabeth Kotowski and published by . This book was released on 2012 with total page 63 pages. Available in PDF, EPUB and Kindle. Book excerpt: Neutron stars have been of interest since Landau proposed their existence in the early 1930's. Soon after, Baade and Zwicky theorized the origins of neutron stars and Tolman, Oppenheimer, and Volkoff modeled neutron stars. It wasn't until until the 1960's when Bell and Hewish found the first pulsar that theoretical neutron stars could be compared to observable results. Since then scientists have found 2000 neutron stars with masses as high as 2 M[circled dot operator]. The models for neutron stars have improved with our understanding of nuclear matter. The equations of state for nuclear matter that describe pressure as a function of energy have been altered for neutron stars. Not all models for nuclear matter fit with neutron star data. This study examines how the models fit the observed masses. The models have been divided into groups based on their treatment of the many body problem. For each model the rotating and non-rotating cases have been examined to see the effects of rotation on the properties of a neutron star at certain masses. Though all neutron stars give insight into super dense matter, this paper will focus on neutron stars near 2 M [circled dot operator] . We see shifts in all properties when moving from the non-rotating to the rotating case. After comparing the resulting masses for each equation of state to the recently found 1.97 [plus or minus] 0.04 M[circled dot operator] neutron star, we can predict the properties of such a massive neutron star. We will also be able to rule out models for the equation of state that do not create large enough stars. About half of the models studied can create non-rotating neutron stars of at least 2.0 M[circled dot operator], while nearly all of the models can create rapidly rotating neutron stars of the same mass.
