scholarly journals Nuclear mass measurements map the structure of atomic nuclei and accreting neutron stars

2020 ◽  
Vol 101 (5) ◽  
Author(s):  
Z. Meisel ◽  
S. George ◽  
S. Ahn ◽  
D. Bazin ◽  
B. A. Brown ◽  
...  
Keyword(s):  
Neutron Stars ◽  
Nuclear Mass ◽  
Mass Measurements ◽  
Atomic Nuclei

scholarly journals Nuclear mass measurements with radioactive ion beams

2019 ◽  
Vol 28 (04) ◽  
pp. 1930005 ◽  
Author(s):  
Michael A. Famiano
Keyword(s):  
Mass Measurement ◽  
Measurement Techniques ◽  
Nuclear Mass ◽  
Mass Measurements ◽  
Future Directions ◽  
Advantages And Disadvantages ◽  
Nuclear Masses ◽  
Under Construction ◽  
Very High ◽  
Practical Constraints

Nuclear masses are the most fundamental of all nuclear properties, yet they can provide a wealth of knowledge, including information on astrophysical sites, constraints on existing theory, and fundamental symmetries. In nearly all applications, it is necessary to measure nuclear masses with very high precision. As mass measurements push to more short-lived and more massive nuclei, the practical constraints on mass measurement techniques become more exacting. Various techniques used to measure nuclear masses, including their advantages and disadvantages are described. Descriptions of some of the world facilities at which the nuclear mass measurements are performed are given, and brief summaries of planned facilities are presented. Future directions are mentioned, and conclusions are presented which provide a possible outlook and emphasis on upcoming plans for nuclear mass measurements at existing facilities, those under construction, and those being planned.

General relativity and neutron stars

2016 ◽  
Vol 31 (02n03) ◽  
pp. 1641017
Author(s):  
D. G. Yakovlev
Keyword(s):  
General Relativity ◽  
Neutron Star ◽  
Neutron Stars ◽  
Gravitational Wave ◽  
Mass Measurements ◽  
Einstein Theory ◽  
Superdense Matter ◽  
Compact Binaries ◽  
Star Models ◽  
Neutron Star Mass

General Relativity affects all major aspects of neutron star structure and evolution including radiation from the surface, neutron star models, evolution in compact binaries. It is widely used for neutron star mass measurements and for studying properties of superdense matter in neutron stars. Observations of neutron stars help testing General Relativity and planning gravitational wave experiments. No deviations from Einstein Theory of Gravity have been detected so far from observations of neutron stars.

scholarly journals Energy of a quantum Coulomb liquid

2019 ◽  
Vol 488 (4) ◽  
pp. 5042-5047 ◽  
Author(s):  
D A Baiko
Keyword(s):  
Heat Capacity ◽  
Neutron Stars ◽  
First Principles ◽  
Thermal Evolution ◽  
Path Integrals ◽  
Strongly Coupled ◽  
Atomic Nuclei ◽  
Metropolis Method ◽  
Dense Fluid ◽  
Crucial Ingredient

ABSTRACT Using the Metropolis method to compute path integrals, the energy of a quantum strongly coupled Coulomb liquid (1 ≤ Γ ≤ 175), composed of distinguishable atomic nuclei and a uniform incompressible electron background, is calculated from first principles. The range of temperatures and densities considered represents fully ionized layers of white dwarfs and neutron stars. In particular, the results allow one to determine reliably the heat capacity of ions in dense fluid stellar matter, which is a crucial ingredient for modelling the thermal evolution of compact degenerate stars.

scholarly journals Examining the nuclear mass surface of Rb and Sr isotopes in the A≈104 region via precision mass measurements

2021 ◽  
Vol 103 (4) ◽  
Author(s):  
I. Mukul ◽  
C. Andreoiu ◽  
J. Bergmann ◽  
M. Brodeur ◽  
T. Brunner ◽  
...  
Keyword(s):  
Sr Isotopes ◽  
Nuclear Mass ◽  
Mass Measurements ◽  
Precision Mass Measurements

scholarly journals Gravitational waves from neutron stars and asteroseismology

2018 ◽  
Vol 376 (2120) ◽  
pp. 20170285 ◽  
Author(s):  
Wynn C. G. Ho
Keyword(s):  
Electromagnetic Wave ◽  
Neutron Stars ◽  
Gravitational Wave ◽  
Gravitational Waves ◽  
Massive Stars ◽  
Supernova Explosion ◽  
Wide Binary ◽  
Fundamental Physics ◽  
Atomic Nuclei ◽  
The Earth

Neutron stars are born in the supernova explosion of massive stars. Neutron stars rotate as stably as atomic clocks and possess densities exceeding that of atomic nuclei and magnetic fields millions to billions of times stronger than those created in laboratories on the Earth. The physical properties of neutron stars are determined by many areas of fundamental physics, and detection of gravitational waves can provide invaluable insights into our understanding of these areas. Here, we describe some of the physics and astrophysics of neutron stars and how traditional electromagnetic wave observations provide clues to the sorts of gravitational waves we expect from these stars. We pay particular attention to neutron star fluid oscillations, examining their impact on electromagnetic and gravitational wave observations when these stars are in a wide binary or isolated system, then during binary inspiral right before merger, and finally at times soon after merger. This article is part of a discussion meeting issue ‘The promises of gravitational-wave astronomy’.

Physics and neutron star interiors

1992 ◽  
Vol 341 (1660) ◽  
pp. 17-27 ◽  
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Dense Matter ◽  
Theoretical Models ◽  
Laboratory Studies ◽  
Neutron Excess ◽  
The Past ◽  
Atomic Nuclei ◽  
Profound Influence ◽  
Important Input

Conditions in neutron stars are more extreme than almost any encountered on Earth: densities exceed those of atomic nuclei, and matter has a large neutron excess. During the past quarter of a century, the challenge of understanding neutron stars has stimulated physicists to confront conditions far different from those normally encountered terrestrially. Laboratory studies have in turn yielded important input for the studies of neutron stars. We discuss a number of examples of this continuing interplay between physics and astrophysics. The first is the equation of state of dense matter, which is the basis for all theoretical models of neutron stars. The second is the composition of dense matter. This has profound influence on neutrino generating processes in neutron stars, and hence on their cooling. A third example is nuclei with a large neutron excess, such as are expected to be present in the crusts of neutron stars. Properties of similar nuclei play an important role in theories of element production.

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