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Constraining The Nuclear Equation Of State From Nuclear Physics And Neutron Star Observations
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Book Synopsis Constraining the Nuclear Equation of State from Nuclear Physics and Neutron Star Observations by : Svenja Kim Greif
Download or read book Constraining the Nuclear Equation of State from Nuclear Physics and Neutron Star Observations written by Svenja Kim Greif and published by . This book was released on 2019 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt:
Book Synopsis Nuclear Equation Of State - Lecture Notes Of The Workshop by : Ahmad Ansari
Download or read book Nuclear Equation Of State - Lecture Notes Of The Workshop written by Ahmad Ansari and published by World Scientific. This book was released on 1996-03-22 with total page 424 pages. Available in PDF, EPUB and Kindle. Book excerpt: In the diversified and changing scenarios of the current frontiers of nuclear physics research, the topic 'Nuclear Equation of State' occupies the pivotal position. The present series of lectures by well known experts in this field span a wide area ranging from low energy to ultrarelativistic energy, with application to astrophysical phenomena like supernovae explosions, neutron star and other stellar processes, phase transitions in quantum chromodynamics, and properties of quark-gluon plasma. The present status of the VUU model for the intermediate energy heavy-ion collisions is also reviewed.
Book Synopsis Sensitivity of Neutron Star Properties to the Equation of State by : Farrooh Fattoyev
Download or read book Sensitivity of Neutron Star Properties to the Equation of State written by Farrooh Fattoyev and published by . This book was released on 2011 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt: ABSTRACT: The subject of this doctoral dissertation is to study the equations of state of nuclear and neutron-star matter. We tackle this problem by employing several models of the relativistic effective interactions. The relativistic effective interactions and their applications to the ground-state properties of medium to heavy nuclei have enjoyed enormous success for the past three decades. With just a few model parameters calibrated to the ground state properties of the closed-shell nuclei, these models exhibit and encode a great amount of physics. However, theses models are untested far away from their narrow window of applicability. In particular, while these models tend to agree on the saturation properties of symmetric nuclear matter, they largely disagree on its density and isospin dependence, especially in the region of high densities and large proton-neutron asymmetries. In order to better understand the properties of nuclear matter at these extreme regions of isospin asymmetry and high-densities, we will apply these models to predict several neutron star properties. Since the matter in the neutron stars are very neutron-rich, while the density of matter in neutron stars spans over a wide range of magnitudes, these compact objects remain unique laboratories for probing the equation of state of neutron-rich matter under conditions unattainable by terrestrial experiments. Thus it is expected that at least the following neutron star properties must be sensitive to the underlying equation of state- maximum mass, typical radii, moments of inertia (both total and crustal), redshifts, and cooling mechanism. We present numerical solutions and in some cases also analytical solutions to each of the properties above. In particular, the sensitivity of the stellar moment of inertia to the neutron-star matter equation of state is examined using accurately-calibrated relativistic mean-field models. We probe this sensitivity by tuning both the density dependence of the symmetry energy and the high density component of the equation of state, properties that are at present poorly constrained by existing laboratory data. Particularly attractive is the study of the fraction of the moment of inertia contained in the solid crust. Analytic treatments of the crustal moment of inertia reveal a high sensitivity to the transition pressure at the core-crust interface. Motivated by a recent astrophysical measurement of the pressure of cold matter above nuclear-matter saturation density, we compute the equation of state of neutron-star matter using various accurately calibrated relativistic models. We found the predictions of these models to be in fairly good agreement with the measured equation of state. In the effort to explain the observational data we introduce a new relativistic effective interaction that is simultaneously constrained by the properties of finite nuclei, their collective excitations, and neutron-star properties. By adjusting two of the empirical parameters of the theory, one can efficiently tune the neutron skin thickness of $^{208}$Pb and the maximum neutron star mass. The new effective interaction is moderately soft at intermediate densities and relatively stiff at high densities. It is fitted to a neutron skin thickness in $^{208}$Pb of only $R_{rm n} - R_{rm p} = 0.16$ fm and a moderately large maximum neutron star mass of 1.94 $M_{rm Sun}$ consistent with the latest observation. Last, theoretical uncertainties in the predictions of relativistic mean-field models are estimated using a chi-square minimization procedure that is implemented by studying the small oscillations around the chi-square minimum. It is shown that such statistical analysis provides access to a wealth of information that would normally remain hidden. The power of covariance analysis is illustrated in two relativistic mean field models. By performing this analysis one obtains meaningful theoretical uncertainties for both model parameters and predicted observables. Moreover, it is shown, how covariance analysis is able to establish robust correlations between physical observables.
Book Synopsis Relativistic Hydrodynamics by : Luciano Rezzolla
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.
Book Synopsis Cosmic Puzzles in Neutron Realms by : Stephen E Dry
Download or read book Cosmic Puzzles in Neutron Realms written by Stephen E Dry and published by . This book was released on 2023-12-21 with total page 0 pages. Available in PDF, EPUB and Kindle. Book excerpt: The holy grail of nuclear physics is the nuclear equation of state. It governs the behavior of nuclear matter at a large variety of densities and proton-neutron asymmetries. In particular for this thesis, I will be focusing on the equation of state for neutron-rich matter, which is perhaps more interesting than symmetric or proton-rich matter because of how much less well it is constrained. The observation of neutron-rich skins in neutron-rich nuclei, such as the doublymagic 208Pb, have helped constrain the equation of state near saturation density ρ0 ≈ 0.16 fm-3. At higher density, neutron stars are prime real estate for observing the neutron-rich equation of state and help us infer important information about the behavior of matter in the most extreme environments.
Book Synopsis Physics of Neutron Stars by : A. M. Kaminker
Download or read book Physics of Neutron Stars written by A. M. Kaminker and published by Nova Biomedical Books. This book was released on 1995 with total page 298 pages. Available in PDF, EPUB and Kindle. Book excerpt: Physics of Neutron Stars
Book Synopsis Nuclear and Particle Astrophysics by :
Download or read book Nuclear and Particle Astrophysics written by and published by . This book was released on 1990 with total page 80 pages. Available in PDF, EPUB and Kindle. Book excerpt: We discuss the physics of matter that is relevant to the structure of compact stars. This includes nuclear, neutron star matter and quark matter and phase transitions between them. Many aspects of neutron star structure and its dependance on a number of physical assumptions about nuclear matter properties and hyperon couplings are investigated. We also discuss the prospects for obtaining constraints on the equation of state from astrophysical sources. Neuron 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 of theory of relativity is correct at the macroscopic scale. 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. Indeed the prompt explosion, from which a constraint had been thought to follow, is now believed not to be mechanism by which most, if any stars, explode. In any case the nuclear equation of state is but one of a multitude on uncertain factors, and possibly one of the least important. The rapid rotation of pulsars is also discussed. It is shown that for periods below a certain limit it becomes increasingly difficult to reconcile them with neutron stars. Strange stars are possible if strange matter is the absolute ground state. We discuss such stars and their compatibility with observation. 112 refs., 37 figs., 6 tabs.
Book Synopsis Neutron Star Crust by : Carlos A. Bertulani
Download or read book Neutron Star Crust written by Carlos A. Bertulani and published by . This book was released on 2013-01-11 with total page 0 pages. Available in PDF, EPUB and Kindle. Book excerpt: Includes bibliographical references and index.
Book Synopsis Nuclear Methods And Nuclear Equation Of State by : Marcello Baldo
Download or read book Nuclear Methods And Nuclear Equation Of State written by Marcello Baldo and published by World Scientific. This book was released on 1999-11-15 with total page 526 pages. Available in PDF, EPUB and Kindle. Book excerpt: The theoretical study of the nuclear equation of state (EOS) is a field of research which deals with most of the fundamental problems of nuclear physics. This book gives an overview of the present status of the microscopic theory of the nuclear EOS. Its aim is essentially twofold: first, to serve as a textbook for students entering the field, by covering the different subjects as exhaustively and didactically as possible; second, to be a reference book for all researchers active in the theory of nuclear matter, by providing a report on the latest developments. Special emphasis is given to the numerous open problems existing at present and the prospects for their possible solutions.The general framework of the different approaches presented in the book is the meson theory of nuclear forces — where no free parameter is introduced — and the many-body treatment of nucleon-nucleon correlations. The ultimate hope of this world-wide effort is the understanding of the structure of nuclear matter, both in the ground state and at finite temperature.The main audience addressed is the community of theoretical nuclear physicists, but nuclear experimentalists and astrophysicists will also find in the book an extensive amount of material of direct interest for their everyday work, particularly for those studying heavy-ion collisions, where the nuclear EOS is of special relevance. Finally, theoretical physicists working on elementary particle theory could find in the book some stimulating ideas and problems directly related to their field.
Book Synopsis Physics of Neutron Star Interiors by : D. Blaschke
Download or read book Physics of Neutron Star Interiors written by D. Blaschke and published by Springer. This book was released on 2008-01-11 with total page 521 pages. Available in PDF, EPUB and Kindle. Book excerpt: Neutron stars are the densest observable bodies in our universe. Born during the gravitational collapse of luminous stars - a birth heralded by spectacular supernova explosions - they open a window on a world where the state of the matter and the strengths of the fields are anything but ordinary. This book is a collection of pedagogical lectures on the theory of neutron stars, and especially their interiors, at the forefront of current research. It addresses graduate students and researchers alike, and should be particularly suitable as a text bridging the gap between standard textbook material and the research literature.
Book Synopsis Nuclear Physics by : National Research Council
Download or read book Nuclear Physics written by National Research Council and published by National Academies Press. This book was released on 1999-03-31 with total page 222 pages. Available in PDF, EPUB and Kindle. Book excerpt: Dramatic progress has been made in all branches of physics since the National Research Council's 1986 decadal survey of the field. The Physics in a New Era series explores these advances and looks ahead to future goals. The series includes assessments of the major subfields and reports on several smaller subfields, and preparation has begun on an overview volume on the unity of physics, its relationships to other fields, and its contributions to national needs. Nuclear Physics is the latest volume of the series. The book describes current activity in understanding nuclear structure and symmetries, the behavior of matter at extreme densities, the role of nuclear physics in astrophysics and cosmology, and the instrumentation and facilities used by the field. It makes recommendations on the resources needed for experimental and theoretical advances in the coming decade.
Book Synopsis Imposing Multi-physics Constraints at Different Densities on the Neutron Star Equation of State by : Suprovo Ghosh
Download or read book Imposing Multi-physics Constraints at Different Densities on the Neutron Star Equation of State written by Suprovo Ghosh and published by . This book was released on 2022 with total page 0 pages. Available in PDF, EPUB and Kindle. Book excerpt: Neutron star matter spans a wide range of densities, from that of nuclei at the surface to exceeding several times normal nuclear matter density in the core. While terrestrial experiments, such as nuclear or heavy-ion collision experiments, provide clues about the behaviour of dense nuclear matter, one must resort to theoretical models of neutron star matter to extrapolate to higher density and finite neutron/proton asymmetry relevant for neutron stars. In this work, we explore the parameter space within the framework of the Relativistic Mean Field model allowed by present uncertainties compatible with state-of-the-art experimental data. We apply a cut-off filter scheme to constrain the parameter space using multi-physics constraints at different density regimes: chiral effective field theory, nuclear and heavy-ion collision data as well as multi-messenger astrophysical observations of neutron stars. Using the results of the study, we investigate possible correlations between nuclear and astrophysical observables.
Book Synopsis The Physics and Astrophysics of Neutron Stars by : Luciano Rezzolla
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 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.
Book Synopsis The Nuclear Equation of State by : Walter Greiner
Download or read book The Nuclear Equation of State written by Walter Greiner and published by Springer Science & Business Media. This book was released on 2013-06-29 with total page 787 pages. Available in PDF, EPUB and Kindle. Book excerpt: The NATO Advanced Study Institute on The Nuclear Equatioo of State was held at Peiiiscola Spain from May 22- June 3, 1989. The school was devoted to the advances, theoretical and experimental, made during the past fifteen years in the physics of nuclear matter under extreme conditions, such as high compression and high temperature. Moie than 300 people had applied for participatio- this demonstrates the tremendous interest in the various subjects presented at the school. Indeed, the topic of this school, namely the Nuclear Equatioo of State, • plays the central role in high energy heavy ion collisions; • contains the intriguing possibilities of various phase transitions (gas - vapor, meson condensation, quark - gluon plasma); • plays an important role in the static and dynamical behavior of stars, especially in supernova explosions and in neutron star stability. The investigation on the nuclear equation of state can only be accomplished in the laboratory by compressing and heating up nuclear matter and the only mechanism known to date to achieve this goal is through shock compression and -heating in violent high energy heavy ion collisions. This key mechanism has been proposed and highly disputed in of high energy heavy ion physics, the early 70's. It plays a central role in the whole field and particularly in our discussions during the two weeks at Peiiiscola.
Book Synopsis Neutron Stars as Laboratories for Fundamental Physics by : Dake Zhou
Download or read book Neutron Stars as Laboratories for Fundamental Physics written by Dake Zhou and published by . This book was released on 2021 with total page 0 pages. Available in PDF, EPUB and Kindle. Book excerpt: This dissertation explores the subatomic world with observations of neutron stars. Neutron stars are exotic and mysterious objects and are placed under the spotlight with current and planned investigations. In the coming decades, multimessenger (electromagnetic, neutrino, gravitational wave and cosmic ray) observations are expected to reveal the physical processes that underlie extreme astrophysical phenomena involving neutron stars such as compact star mergers and core-collapse supernovae. These observations could provide new insights about particle and nuclear physics under extreme conditions and physics beyond the standard model. Open questions concerning ab initio nuclear theory, dense quantum chromodynamics matter and the nature of dark matter are summarized. Following a brief review of neutron stars, the prospect of constraining neutron matter equation of state with future gravitational wave detections is examined. The rest of the thesis focuses on potential neutron star observables and constraints of a few emerging dark matter models. It is shown that dark baryons lighter than ~ 1.2 GeV are incompatible with observed massive pulsars. A scenario where effects of self-interacting dark matter may be detected via gravitational waves from binary neutron star mergers is studied. Finally, the closing chapter investigates impacts and potential observable signatures of a novel superfluid phase of matter arising from neutrino-portal scalars carrying lepton numbers in newly-born neutron stars.
Book Synopsis Constraints on the Neutron Equation of State Using the Difference in 54Ni-54Fe Mirror Pair Charge Radii by : Skyy Venancio Pineda
Download or read book Constraints on the Neutron Equation of State Using the Difference in 54Ni-54Fe Mirror Pair Charge Radii written by Skyy Venancio Pineda and published by . This book was released on 2022 with total page 0 pages. Available in PDF, EPUB and Kindle. Book excerpt: Just like the ideal gas law is used to characterize a `perfect' gas, equations of state can be used to describe nuclear matter. Two such equations of state include the symmetric matter equation of state and the neutron matter equation of state. While symmetric matter is well known, neutron matter is not, especially when extrapolating to higher densities. The nuclear matter equation of state is of interest because a greater understanding of it is required to predict properties of both super-heavy nuclei and neutron stars. There is ongoing debate about whether the neutron equation of state is `soft' or `stiff', where a `stiff' equation of state implies the pressure in the nucleus increases rapidly with increasing density and consequently implies a larger neutron star radius. A way to constrain this neutron equation of state is through the slope of the symmetry energy (the $L$ parameter), where the symmetry energy is the difference between the symmetric and neutron matter equations of state. Conceptually, $L$ is proportional to the pressure of pure neutron matter at a specific density, and can also be thought of as a restoration force (`spring constant') between protons and neutrons when they are dislocated in the nucleus.The complication is that $L$ is not a physical observable and cannot be directly measured in the laboratory. However, it has been shown that the neutron skin thickness ($\Delta R_\mathrm{np}$) of neutron-rich nuclei are correlated to $L$. By measuring the neutron skin we can therefor place constraints on the $L$ parameter and ultimately the neutron equation of state. Many experimental and theoretical techniques have been used to constrain $L$. It is noted that all of them are model-dependent in some way. Even though many of these analyses agree within $1\sigma$, they each have tendencies toward either the `soft' or the `stiff' nuclear equation of state. Results from the PREX and CREX experiments, highly regarded benchmarks for the neutron skin value, also show tension between their results, highlighting that discretion is needed when addressing the model-dependent components in these analyses. This model-dependence brings about the need for increased systematic measurements of the $L$ parameter to add to the discussion on constraints on $L$.The difference in charge radii ($\Delta R_\mathrm{ch}$) is a new, purely electromagnetic probe to deduce the neutron skin and constrain $L$. Assuming perfect charge symmetry, the distribution of the protons is equal to the distribution of the neutrons in the mirror nucleus. By taking the difference in charge radii, the neutron skin can be obtained. In reality, however, the charge symmetry is broken by the Coulomb interaction that pushes protons out relative to neutrons, leading to a weaker correlation between $\Delta R_\mathrm{np}$ and $\Delta R_\mathrm{ch}$. However, even with this Coulomb disruption, $\Delta R_\mathrm{ch}$ shows tighter correlation to $L$ than that of $\Delta R_\mathrm{np}$. It was also shown that $\Delta R_\mathrm{ch}$ is correlated to $|N-Z| \times L$. Due to this correlation, ideally a mirror pair would be chosen with a high $|N-Z|$ to provide a tighter constraint, where the maximum possible is $|N-Z|=6$ for the $^{22}$Si-$^{22}$O pair. The present $^{54}\mathrm{Ni}$-$^{54}\mathrm{Fe}$ mirror pair has a rather low $|N-Z|=2$, and therefor requires a highly sensitive technique to be able to provide good enough results to place constraints on $L$, otherwise too large of an uncertainty would void any meaningful discussion.Isotope shift measurements using bunched beam collinear laser spectroscopy of $^{54}$Ni ($I^\pi=0^+,\,\,t_{1/2}=114\,\mathrm{ms}$) and other nickel isotopes were performed at the BEam COoling and LAser spectroscopy (BECOLA) facility at the National Superconducting Cyclotron Laboratory (NSCL) at Michigan State University. These precise measurements were used to extract the charge radius for $^{54}$Ni for the first time to be $R(^{54}\mathrm{Ni})=3.737 \pm 0.003$\,fm. Using the already known $^{54}$Fe charge radius from literature, the difference in charge radii between the mirror pairs was taken in order to obtain $\Delta R_\mathrm{ch}=0.049 \pm 0.004$\,fm. Based on the correlation between $L$ and $\Delta R_\mathrm{ch}$ calculated by density functional theory using the Skyrme energy density functional, the present $\Delta R_\mathrm{ch}(A=54)$ set a constraint on the $L$ parameter as $21 \le L \le 88$\,MeV. The model takes into account corrections for the quadrupole deformation, which was evaluated through the $\beta_2$ deformation parameter obtained by the reduced $E2$ transition probability $B(E2,\uparrow)$ for $^{54}$Ni.These constraints on $L$ from BECOLA are in good agreement with the GW170817 neutron star merger, whose results also favor the `soft' neutron equation of state, providing an link between a new terrestrial-based experimental method and an astrophysical observation. These results are different from the PREX results, which favor the `stiff' EOS. To add to the systematics, the same method using parity violating electron scattering to measure the electroweak form factor was used with the CREX experiment.Using the $\Delta R_\mathrm{ch}$ method has also enabled constraints on the neutron skin for $^{48}$Ca which agree with the CREX results. The tension between CREX and PREX stems from the model-dependent step during the analyses demonstrated by a reevaluation of the PREX results which resulted in a smaller neutron skin and $L$ value consistent with GW170817, BECOLA, and CREX.A global trend analysis evaluated the relationship between $\Delta R_\mathrm{ch}$ and $L$. The results concluded that while there was correlation between the observable and the $L$ parameter, it could not place stringent constrains on the neutron equation of state within the model, hearkening back to model-dependence playing a critical role in the determination of $L$.