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Author: Steven Patrick Harris Publisher: ISBN: Category : Electronic dissertations Languages : en Pages : 183
Book Description
Neutron star mergers are the only situation in nature in which we find matter compressed to several times nuclear saturation density and temperatures of several tens of MeV. By observing and numerically simulating neutron star mergers, we can learn about the nature of matter at high temperatures and densities. Neutron star merger simulations evolve Einstein's equations of general relativity coupled to the equations of relativistic hydrodynamics along with a nuclear equation of state, which describes the neutron star matter. Many simulations also take into account neutrino transport and electrodynamics. The purpose of this thesis is to see whether other physical processes, including thermal transport and viscosity, are relevant to neutron star mergers and thus should be included in merger simulations. After an introduction to the QCD phase diagram, the nuclear equations of state, and neutron star mergers, I discuss three projects related to transport and nuclear matter in neutron star mergers. The first is the nature of beta equilibrium in the portion of a merger that is transparent to neutrinos. We calculate the weak interaction (Urca) rates and find that the beta equilibrium condition needs to be modified by adding an additional chemical potential, which changes slightly the particle content in neutrino-transparent beta equilibrium. Secondly, we calculate the bulk viscosity in neutrino-transparent nuclear matter in conditions encountered in neutron star mergers. Bulk viscosity arises from a phase lag between the pressure and density in the nuclear matter, which is due to the finite rate of beta equilibration. When bulk viscosity is sufficiently strong, which happens when the equilibration rate nearly matches the frequency of the density oscillation, it can noticeably dampen the oscillation. We find that in certain thermodynamic conditions likely encountered in mergers, oscillations in nuclear matter can be damped on timescales on the order of 10 milliseconds, so we conclude that bulk viscosity should be included in merger simulations. Finally, we study thermal transport due to axions in neutron star mergers. We conclude that axions are never trapped in mergers, but instead escape, carrying energy away from the merger. We calculate the cooling time due to the energy carried away by axions and find that within current constraints on the axion-nucleon coupling, axions could cool fluid elements in mergers on timescales which could affect the dynamics of the merger.
Author: Steven Patrick Harris Publisher: ISBN: Category : Electronic dissertations Languages : en Pages : 183
Book Description
Neutron star mergers are the only situation in nature in which we find matter compressed to several times nuclear saturation density and temperatures of several tens of MeV. By observing and numerically simulating neutron star mergers, we can learn about the nature of matter at high temperatures and densities. Neutron star merger simulations evolve Einstein's equations of general relativity coupled to the equations of relativistic hydrodynamics along with a nuclear equation of state, which describes the neutron star matter. Many simulations also take into account neutrino transport and electrodynamics. The purpose of this thesis is to see whether other physical processes, including thermal transport and viscosity, are relevant to neutron star mergers and thus should be included in merger simulations. After an introduction to the QCD phase diagram, the nuclear equations of state, and neutron star mergers, I discuss three projects related to transport and nuclear matter in neutron star mergers. The first is the nature of beta equilibrium in the portion of a merger that is transparent to neutrinos. We calculate the weak interaction (Urca) rates and find that the beta equilibrium condition needs to be modified by adding an additional chemical potential, which changes slightly the particle content in neutrino-transparent beta equilibrium. Secondly, we calculate the bulk viscosity in neutrino-transparent nuclear matter in conditions encountered in neutron star mergers. Bulk viscosity arises from a phase lag between the pressure and density in the nuclear matter, which is due to the finite rate of beta equilibration. When bulk viscosity is sufficiently strong, which happens when the equilibration rate nearly matches the frequency of the density oscillation, it can noticeably dampen the oscillation. We find that in certain thermodynamic conditions likely encountered in mergers, oscillations in nuclear matter can be damped on timescales on the order of 10 milliseconds, so we conclude that bulk viscosity should be included in merger simulations. Finally, we study thermal transport due to axions in neutron star mergers. We conclude that axions are never trapped in mergers, but instead escape, carrying energy away from the merger. We calculate the cooling time due to the energy carried away by axions and find that within current constraints on the axion-nucleon coupling, axions could cool fluid elements in mergers on timescales which could affect the dynamics of the merger.
Author: Praveen Manoharan Publisher: ISBN: 9783658368425 Category : Languages : en Pages : 0
Book Description
In the last 25 years, an extensive body of work has developed various equation of state independent - or (approximately) universal - relations that allow for the inference of neutron star parameters from gravitational wave observations. These works, however, have mostly been focused on singular neutron stars, while our observational efforts at the present, and in the near future, will be focused on binary neutron star (BNS) mergers. In light of these circumstances, the last five years have also given rise to more attempts at developing universal relations that relate BNS pre-merger neutron stars to stellar parameters of the post-merger object, mostly driven by numerical relativity simulations. In this thesis a first attempt at perturbatively deriving universal relations for binary neutron star mergers with long-lived neutron star remnants is presented. The author succeeds in confirming previous results relating pre-merger binary tidal deformabilities to the f-mode frequency of the post-merger object. Combining this result with recent advances of computing the f-mode frequency of fast rotating neutron stars, he also derives a combined relation that relates the pre-merger binary tidal deformability of a BNS to the effective compactness of a long-lived neutron star remnant. Finally, he also proposes a direct relation between these quantities with improved accuracy. About the author Praveen Manoharan is PhD student at Tübingen University, Institute for Theoretical Astrophysics.
Author: Luciano Rezzolla Publisher: Springer ISBN: 3319976168 Category : Science Languages : en Pages : 811
Book Description
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).
Author: Ramadan M. Kuridan Publisher: Springer Nature ISBN: 3031269322 Category : Science Languages : en Pages : 284
Book Description
This textbook provides a thorough explanation of the physical concepts and presents the general theory of different forms through approximations of the neutron transport processes in nuclear reactors and emphasize the numerical computing methods that lead to the prediction of neutron behavior. Detailed derivations and thorough discussions are the prominent features of this book unlike the brevity and conciseness which are the characteristic of most available textbooks on the subject where students find them difficult to follow. This conclusion has been reached from the experience gained through decades of teaching. The topics covered in this book are suitable for senior undergraduate and graduate students in the fields of nuclear engineering and physics. Other engineering and science students may find the construction and methodology of tackling problems as presented in this book appealing from which they can benefit in solving other problems numerically. The book provides access to a one dimensional, two energy group neutron diffusion program including a user manual, examples, and test problems for student practice. An option of a Matlab user interface is also available.
Author: Vsevolod Nedora Publisher: ISBN: Category : Languages : en Pages : 0
Book Description
In August 2017, a merger of two neutron stars (NSs) was detected for the first time via several carriers. Observed in gravitational waves, as well as in the electromagnetic spectrum, the GW170817 marked the dawn of multi-messenger astronomy for compact object mergers, and shed light on numerous astrophysical aspects of binary neutron star (BNS) mergers and on the properties of matter at supranuclear densities. And yet many questions remain, starting with the outcome of the merger. Was it a massive NS temporarily supported against collapse, or a black hole? How important are BNS mergers in cosmic chemical evolution, i.e., the evolution of spatial and temporal distributions of heavy elements in galaxies? It is known that they enrich their surroundings with very heavy elements, but are they the dominant source of these elements? Modeling these events on the computer, do we understand them correctly, i.e., do our predictions regarding the properties of the ejected matter and its EM signatures agree with the newly gained data? This thesis is dedicated to addressing these questions by means of analyzing a large set of numerical simulations of BNS mergers, performed with state-of-the-art numerical tools, and targeted specifically to GW170817. Employing a suite of postprocessing tools we study the matter dynamics. Special attention is given to matter, ejected from the system during and after merger, so-called ejecta. With the help of a parameterized nucleosynthesis model, we study the final abundances of heavy elements in ejecta, comparing them to solar abundances. Furthermore, we investigate EM emission, powered by the decay of newly synthesized heavy elements, comparing it to the observations of GW170817. Finally, we study the long-term emission of the ejected material as it propagates through the interstellar medium (ISM), via our new numerical tools, comparing the results with a recently detected change in the emission from GW170817.
Author: Steven Patrick Harris
Author: Steven Patrick Harris
Author: Oliver Just
Author: Praveen Manoharan
Author: Antonio M. Gentile
Author: Luciano Rezzolla
Author: 
Author: Ramadan M. Kuridan
Author: Alex James Wright
Author: Jin-Fuw Lee
Author: Vsevolod Nedora