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Author: Enping Zhou
Publisher: Springer Nature
ISBN: 9811541515
Category : Science
Languages : en
Pages : 93
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Book Description
This book focuses on the equation of state (EoS) of compact stars, particularly the intriguing possibility of the “quark star model.” The EoS of compact stars is the subject of ongoing debates among astrophysicists and particle physicists, due to the non-perturbative property of strong interaction at low energy scales. The book investigates the tidal deformability and maximum mass of rotating quark stars and triaxially rotating quark stars, and compares them with those of neutron stars to reveal significant differences. Lastly, by combining the latest observations of GW170817, the book suggests potential ways to distinguish between the neutron star and quark star models.
Author: Enping Zhou
Publisher: Springer Nature
ISBN: 9811541515
Category : Science
Languages : en
Pages : 93
Get Book Here
Book Description
This book focuses on the equation of state (EoS) of compact stars, particularly the intriguing possibility of the “quark star model.” The EoS of compact stars is the subject of ongoing debates among astrophysicists and particle physicists, due to the non-perturbative property of strong interaction at low energy scales. The book investigates the tidal deformability and maximum mass of rotating quark stars and triaxially rotating quark stars, and compares them with those of neutron stars to reveal significant differences. Lastly, by combining the latest observations of GW170817, the book suggests potential ways to distinguish between the neutron star and quark star models.
Author: John L. Friedman
Publisher: Cambridge University Press
ISBN: 1107310601
Category : Science
Languages : en
Pages : 435
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Book Description
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.
Author: Jeffrey L. Peterson
Publisher:
ISBN:
Category :
Languages : en
Pages : 0
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Book Description
Compact stars (CSs) are the remnants of "dead" stars that were too small to form black holes; the category includes both white dwarfs (WDs) and neutron stars (NSs). To produce a full description of any magnetized compact star requires solving Einstein's equations in unison with Maxwell's equations. However, when putting these two sets of equations together, there is an additional degree of freedom that requires the inclusion of the equation of state (EOS) of the stellar matter in question. The most notable difference between CSs and other stars is that CSs consist of degenerate fermion matter. Fermionic matter exists in a degenerate state when the temperature is low compared to the Fermi energy. Such states arise due to the Pauli exclusion principle, which states that no two identical fermions (particles with half integer spin) in the same quantum system may inhabit the same quantum state. In the case of WDs, this degeneracy is caused solely by electrons; whereas, in NSs, the degeneracy is in several species of particles including neutrons and protons, but also more "exotic" baryons, such as Lambdas, Sigmas, and Cascades. In the grand canonical ensemble, the stellar EOS is typically expressed as the relation between the total energy density of a gas of particles and their pressure. It is calculated using thermodynamics with, in the NS case, an additional contribution from the strong nuclear force, which must be modeled. Due to computational difficulty, the EOS is often calculated in a simplified way, assuming that one aspect or another is not significant. As such, EOSs exist with temperature effects or with magnetic field effects, but not with both. For example, higher temperatures (without additional degrees of freedom) lead to higher pressures at the same energy density; the EOS is "stiffer." Magnetic fields lead to a pressure anisotropy and Landau quantization, which gives rise to De Haas-Van Alphen oscillations in the EOS. This thesis breaks new ground by simultaneously including both temperature and magnetic field effects into the EOS of compact stars. The thermodynamic portion of the EOS is calculated by treating the particles as a relativistic free Fermi gas, in which, particles are treated as non-interacting and must obey Fermi-Dirac statistics. This approach also allows for the calculation of other thermodynamic quantities, such as number density, entropy density, and magnetization. Contributions from the strong force are calculated using the chiral mean field (CMF) model for neutron stars. The CMF model is a relativistic effective model based on a non-linear realization of the linear sigma model of Quantum Chromodynamics (QCD). It features hadron deconfinement into quarks and self-consistent chiral symmetry restoration. Each fundamental force is thought to have a force carrying boson (particles with integer spin, not subject to Pauli exclusion). The photon is the carrier for the electromagnetic force and the carrier for the strong nuclear force is the gluon. In the CMF model, gluons are approximated as "mesons," which are exchanged between hadrons and quarks. As a result, these mesons acquire some properties from both gluons and quarks. Note that, due to the high density and low temperature of NS matter, standard QCD approaches fail to provide an adequate description. Lattice QCD exhibits the sign problem at non-zero baryon density, due to integrating highly oscillating functions. Perturbative QCD breaks down in the presence of strong particle interactions. These are both conditions found in NSs. Finally, this thesis investigates the EOS for isospin-symmetric matter (equal numbers of protons and neutrons or up and down quarks), to reproduce conditions found in heavy ion collisions (HICs). While HICs do not create matter with net density comparable to that of CSs, the energy density is comparable to that of CSs due to their relativistic speeds. This makes HICs the closest we can get to creating CS matter on Earth.
Author: Jaime Klapp
Publisher: Springer Science & Business Media
ISBN: 3642277225
Category : Science
Languages : en
Pages : 528
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Book Description
The book contains invited lectures and selected contributions presented at the Enzo Levi and XVII Annual Meeting of the Fluid Dynamic Division of the Mexican Physical Society in 2011. It is aimed to fourth year undergraduate and graduate students, and scientists in the field of physics, engineering and chemistry that have interest in Fluid Dynamics from the experimental and theoretical point of view. The invited lectures are introductory and avoid the use of complicate mathematics. The other selected contributions are also adequate to fourth year undergraduate and graduate students. The Fluid Dynamics applications include multiphase flow, convection, diffusion, heat transfer, rheology, granular material, viscous flow, porous media flow, geophysics and astrophysics. The material contained in the book includes recent advances in experimental and theoretical fluid dynamics and is adequate for both teaching and research.
Author: I͡Akov Borisovich Zelʹdovich
Publisher:
ISBN: 9780226979557
Category : Astrophysics
Languages : en
Pages : 718
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Book Description
Author: U. Esser
Publisher: Springer Science & Business Media
ISBN: 3662123649
Category : Science
Languages : en
Pages : 1266
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Book Description
From the reviews: "Astronomy and Astrophysics Abstracts has appeared in semi-annual volumes since 1969 and it has already become one of the fundamental publications in the fields of astronomy, astrophysics and neighbouring sciences. It is the most important English-language abstracting journal in the mentioned branches. ...The abstracts are classified under more than a hundred subject categories, thus permitting a quick survey of the whole extended material. The AAA is a valuable and important publication for all students and scientists working in the fields of astronomy and related sciences. As such it represents a necessary ingredient of any astronomical library all over the world." Space Science Reviews#1 "Dividing the whole field plus related subjects into 108 categories, each work is numbered and most are accompanied by brief abstracts. Fairly comprehensive cross-referencing links relevant papers to more than one category, and exhaustive author and subject indices are to be found at the back, making the catalogues easy to use. The series appears to be so complete in its coverage and always less than a year out of date that I shall certainly have to make a little more space on those shelves for future volumes." The Observatory Magazine#2
Author:
Publisher:
ISBN:
Category : Nuclear energy
Languages : en
Pages : 612
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Book Description
Author: Astronomisches Rechen-Institut
Publisher: Springer Science & Business Media
ISBN: 3662123762
Category : Science
Languages : en
Pages : 1592
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Book Description
"Astronomy and Astrophysics Abstracts" appearing twice a year has become oneof the fundamental publications in the fields of astronomy, astrophysics andneighbouring sciences. It is the most important English-language abstracting journal in the mentioned branches. The abstrats are classified under more than a hundred subject categories, thus permitting a quick survey of the whole extended material. The AAA is a valuable and important publication for all students and scientists working in the fields of astronomy and related sciences. As such it represents a necessary ingredient of any astronomical library all over the world.
Author:
Publisher:
ISBN:
Category : Aeronautics
Languages : en
Pages : 892
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Book Description
Author: Peter O. Hess
Publisher: Springer
ISBN: 3319250612
Category : Science
Languages : en
Pages : 263
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Book Description
This book explores the role of singularities in general relativity (GR): The theory predicts that when a sufficient large mass collapses, no known force is able to stop it until all mass is concentrated at a point. The question arises, whether an acceptable physical theory should have a singularity, not even a coordinate singularity. The appearance of a singularity shows the limitations of the theory. In GR this limitation is the strong gravitational force acting near and at a super-massive concentration of a central mass. First, a historical overview is given, on former attempts to extend GR (which includes Einstein himself), all with distinct motivations. It will be shown that the only possible algebraic extension is to introduce pseudo-complex (pc) coordinates, otherwise for weak gravitational fields non-physical ghost solutions appear. Thus, the need to use pc-variables. We will see, that the theory contains a minimal length, with important consequences. After that, the pc-GR is formulated and compared to the former attempts. A new variational principle is introduced, which requires in the Einstein equations an additional contribution. Alternatively, the standard variational principle can be applied, but one has to introduce a constraint with the same former results. The additional contribution will be associated to vacuum fluctuation, whose dependence on the radial distance can be approximately obtained, using semi-classical Quantum Mechanics. The main point is that pc-GR predicts that mass not only curves the space but also changes the vacuum structure of the space itself. In the following chapters, the minimal length will be set to zero, due to its smallness. Nevertheless, the pc-GR will keep a remnant of the pc-description, namely that the appearance of a term, which we may call "dark energy", is inevitable. The first application will be discussed in chapter 3, namely solutions of central mass distributions. For a non-rotating massive object it is the pc-Schwarzschild solution, for a rotating massive object the pc-Kerr solution and for a charged massive object it will be the Reissner-Nordström solution. This chapter serves to become familiar on how to resolve problems in pc-GR and on how to interpret the results. One of the main consequences is, that we can eliminate the event horizon and thus there will be no black holes. The huge massive objects in the center of nearly any galaxy and the so-called galactic black holes are within pc-GR still there, but with the absence of an event horizon! Chapter 4 gives another application of the theory, namely the Robertson-Walker solution, which we use to model different outcomes of the evolution of the universe. Finally the capability of this theory to predict new phenomena is illustrated.
