Neutrino, Nucleosynthesis in Neutron Star Mergers and Multi-messenger Observation PDF Download

Author: Yonglin Zhu
Publisher:
ISBN:
Category :
Languages : en
Pages : 120

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Author: Debades Bandyopadhyay
Publisher: Springer
ISBN: 9783030951733
Category : Science
Languages : en
Pages : 0

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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.

Author: Luciano Rezzolla
Publisher: Springer
ISBN: 3319976168
Category : Science
Languages : en
Pages : 811

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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: Vsevolod Nedora
Publisher:
ISBN:
Category :
Languages : en
Pages : 0

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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:
Publisher:
ISBN:
Category :
Languages : en
Pages :

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Author: Alessandro De Angelis
Publisher: Springer
ISBN: 3319781812
Category : Science
Languages : en
Pages : 733

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This book introduces particle physics, astrophysics and cosmology. Starting from an experimental perspective, it provides a unified view of these fields that reflects the very rapid advances being made. This new edition has a number of improvements and has been updated to describe the recent discovery of gravitational waves and astrophysical neutrinos, which started the new era of multimessenger astrophysics; it also includes new results on the Higgs particle. Astroparticle and particle physics share a common problem: we still don’t have a description of the main ingredients of the Universe from the point of view of its energy budget. Addressing these fascinating issues, and offering a balanced introduction to particle and astroparticle physics that requires only a basic understanding of quantum and classical physics, this book is a valuable resource, particularly for advanced undergraduate students and for those embarking on graduate courses. It includes exercises that offer readers practical insights. It can be used equally well as a self-study book, a reference and a textbook.

Author: Vsevolod Nedora
Publisher:
ISBN:
Category :
Languages : en
Pages : 0

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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: Chengchao Yuan
Publisher:
ISBN:
Category :
Languages : en
Pages : 0

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The historical coincident detection of gravitational waves (GWs) and electromagnetic (EM) counterparts from the binary neutron star merger event GW 170817 heralds a new era in multi-messenger astronomy. At the same time, since the first discovery of the high-energy astrophysical neutrinos in 2012 by IceCube, neutrino astrophysics has made significant progress and has started playing an increasingly important role in multi-messenger analyses. We are currently in the stage where we can probe the nature of the extreme astrophysical phenomena with the synergies between EM photons, neutrinos, GWs, and cosmic rays. In this dissertation, I start with an overview of the development of multi-messenger astrophysics and its application to astrophysical mergers. I will present our work on the cumulative diffuse neutrino background from galaxy/cluster mergers and show that our scenario can explain the diffuse neutrino flux without violating the extragalactic gamma-ray background constraints (chapter 2). We further demonstrate that the synchrotron and inverse Compton emissions produced by secondary electrons/positrons are consistent with the radio and X-ray observations of merging galaxies such as NGC 660 and NGC 3256 (chapter 3). In chapters 4 & 5, we focus on the jet-induced neutrino and EM counterparts from supermassive black hole (SMBH) mergers subsequent to GW radiation and discuss the detection perspectives for the ongoing and next-generation neutrino, optical, and GW missions. The short gamma-ray bursts, which are generally thought to arise from compact binary object (CBO) mergers, could be promising candidates for multi-messenger studies. We then consider a special scenario where short GRBs are embedded in disks of active galactic nuclei (AGN) and investigate their GeV signatures in chapter 6. In a separate effort, we study the stacking and multiplet constraints on the blazar contribution to the cumulative diffuse neutrino flux, assuming a generic relationship between neutrino and gamma-ray luminosities (chapter 7). We show that these two limits are complementary, and our results support the argument that blazars are disfavored as the dominant sources of the 100-TeV neutrino background. This work provides rather general and stringent constraints for future studies of blazar neutrinos.

Author: Steven Patrick Harris
Publisher:
ISBN:
Category : Electronic dissertations
Languages : en
Pages : 183

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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: J.E Ventura
Publisher: Springer Science & Business Media
ISBN: 9780792313977
Category : Science
Languages : en
Pages : 616

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Some twenty-three years after the discovery of pulsars and their identification as rotating neutron stars, neutron star physics may be regarded as comingofage. Pul sars and accreting neutron stars have now been studied at every wavelength, from the initial radio observations, through optical, X-, and "{-ray, up to the very recent observations in the TeV region, while theorists have studied in some detail relevant physical processes both outside and inside neutron stars. As a result, comparisonof theory with observation provides a test ofour theoretical ideas in fields as diverse as neutron and nuclear matter, superfluidity and superconductivity, the acceleration of high energy particles, and the generation and maintenance of intense magnetic fields. For example, through observations of glitches and post glitch behavior of pulsars, it has become possible to establish the presence ofsuperfluid neutron mat ter in the inner crust of neutron stars, and to determine some of its properties, while neutron stars in compact binary systems offer one ofthe most efficient energy generation mechanisms known. It is in fact the interactive interpretation of these ,diverse pieces of information that can lead to major advances in our understanding of the physics of these exotic objects, and justifies the characterization of neutron stars as hadron physics laboratories.