scholarly journals Total energy in supernova neutrinos and the tidal deformability and binding energy of neutron stars

2020 ◽  
Vol 102 (10) ◽  
Author(s):  
Brendan Reed ◽  
C. J. Horowitz
Keyword(s):  
Binding Energy ◽  
Total Energy ◽  
Neutron Stars ◽  
Supernova Neutrinos

scholarly journals NEUTRON STARS AND THE FERMIONIC CASIMIR EFFECT

2002 ◽  
Vol 17 (06n07) ◽  
pp. 1059-1064 ◽  
Author(s):  
PIOTR MAGIERSKI ◽  
AUREL BULGAC ◽  
PAUL-HENRI HEENEN
Keyword(s):  
Total Energy ◽  
Neutron Stars ◽  
Crystal Lattice ◽  
Coulomb Interaction ◽  
Quantum Correction ◽  
Casimir Effect ◽  
Casimir Energy ◽  
Large Influence

The inner crust of neutron stars consists of nuclei of various shapes immersed in a neutron gas and stabilized by the Coulomb interaction in the form of a crystal lattice. The scattering of neutrons on nuclear inhomegeneities leads to the quantum correction to the total energy of the system. This correction resemble the Casimir energy and turn out to have a large influence on the structure of the crust.

QUADRONIUM: UNRAVELLING THE e+e− PUZZLE

1991 ◽  
Vol 06 (11) ◽  
pp. 1985-2004 ◽  
Author(s):  
JAMES J. GRIFFIN
Keyword(s):  
Binding Energy ◽  
Total Energy ◽  
Production Process ◽  
Internal Structure ◽  
Heavy Ion ◽  
Two Stage ◽  
Strong Binding ◽  
Positron Emission

The development of the Quadronium scenario for the e+e− puzzle is reviewed. The Quadronium (strong binding) hypothesis leads to a two-stage (spontaneous creation)/(energy inflation) production process for Q0, which can yield decay lines as narrow in energy as those observed, and which suggests that Q0 may either be created free, or bound to an outgoing heavy ion. In turn, this bound/free dichotomy provides a template for analyzing the experimental facts, which yields a good semiquantitative description of the EPOS data. Remarkably, this description of the later stages of the process is independent of the internal structure of the decaying object, and yet provides predictions for much of the available data. Finally, the bound decays imply a new (and so far never studied) process of sharp annihilative positron emission (SAPosE), in which the electron is captured into a Bohr — Dirac orbit of the nuclear ion, and the positron emerges with a total energy equal to the energy of the decaying Q0 state plus the binding energy of the electron. These successes focus the attention on the underlying hypothesis: How can one prove definitively either that Q0 is or is not strongly bound?

scholarly journals Measuring the neutron star compactness and binding energy with supernova neutrinos

2017 ◽  
Vol 2017 (11) ◽  
pp. 036-036 ◽  
Author(s):  
Andrea Gallo Rosso ◽  
Francesco Vissani ◽  
Maria Cristina Volpe
Keyword(s):  
Neutron Star ◽  
Binding Energy ◽  
Supernova Neutrinos

EFFECTS OF IN-MEDIUM MODIFICATION OF WEAKLY INTERACTING LIGHT BOSON MASS IN NEUTRON STARS

2011 ◽  
Vol 26 (05) ◽  
pp. 367-375 ◽  
Author(s):  
A. SULAKSONO ◽  
MARLIANA ◽  
KASMUDIN
Keyword(s):  
Neutron Star ◽  
Binding Energy ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Observational Data ◽  
Boson Mass ◽  
Characteristic Scale ◽  
Neutron Star Matter ◽  
Weakly Interacting ◽  
Medium Modification

The effects of the presence of weakly interacting light boson (WILB) in neutron star matter have been revisited. Direct checking based on the experimental range of symmetric nuclear matter binding energy1 and the fact that the presence of this boson should give no observed effect on the crust properties of neutron star matter, shows that the characteristic scale of WILB [Formula: see text] should be ≤2 GeV-2. The recent observational data with significant low neutron stars radii2 and the recent largest pulsar which has been precisely measured, i.e. J1903+0327 (Ref. 3) indicate that in-medium modification of WILB mass in neutron stars cannot be neglected.

Molecular Dynamics Simulations of Polypropylene and Talcum Nanocomposite

2012 ◽  
Vol 466-467 ◽  
pp. 161-164
Author(s):  
Na Song ◽  
Qing Wang ◽  
Xiao Ji Zhang ◽  
Peng Ding
Keyword(s):  
Molecular Dynamics ◽  
Molecular Modeling ◽  
Binding Energy ◽  
Potential Energy ◽  
Total Energy ◽  
Polymer Chains ◽  
Nanocomposite System ◽  
Modeling Techniques ◽  
Dynamics Simulations ◽  
Simulation Time

Molecular modeling techniques were applied to predicting binding energy for PP/talc and PP-MAH/talc. A supercell containing talc and two polymer chains of 25 repeating units length was constructed. The COMPASS forcefield has been used to represent the interactions in the nanocomposite system. The interactions are improved between the polymer and the clay in the presence of functional groups. And the total energy and potential energy between PP and the talc decreases almost linearly with the simulation time.

Hydrogen adsorbed in ab initio computationally simulated nanoporous carbon. An energetics study

2007 ◽  
Vol 1042 ◽  
Author(s):  
R. M. Valladares ◽  
Alexander Valladares ◽  
A. G. Calles ◽  
Ariel A. Valladares
Keyword(s):  
Hydrogen Atom ◽  
Binding Energy ◽  
Total Energy ◽  
Ab Initio ◽  
Molecular Hydrogen ◽  
Molecular Form ◽  
Average Energy ◽  
Nanoporous Carbon ◽  
Hydrogen Atoms ◽  
Pure Carbon

AbstractNanoporous carbon has been considered an interesting and potentially useful material for storing hydrogen. Using nanoporous carbon periodic supercells with 216 atoms and 50 % porosity, constructed with a novel ab initio approach devised by us, the dangling bonds of the carbon atoms were first saturated with hydrogen, then relaxed and its total energy calculated with and without hydrogen. Next the same number of hydrogen atoms, in molecular form, was randomly placed within the pore of the pure carbon supercell, then the sample relaxed, and finally its total energy calculated, also with and without hydrogens. From these results the average energy per hydrogen atom is obtained for both cases. For the molecular hydrogen sample the binding energy found per hydrogen atom is 343.89 meV, which compares favourably with values reported in the literature, 300-400 meV/molecule.

A FINITE NUCLEON EXTENDED VOLUME MODEL FOR NUCLEAR MATTER

2011 ◽  
Vol 20 (supp02) ◽  
pp. 160-167 ◽  
Author(s):  
ALBERTO S. S. ROCHA ◽  
CÉSAR A. Z. VASCONCELLOS ◽  
HELIO T. COELHO
Keyword(s):  
Binding Energy ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Finite Volume ◽  
Nuclear Physics ◽  
Exchange Interactions ◽  
Meson Exchange ◽  
Volume Model ◽  
Relativistic Approximation ◽  
Experimental Values

We investigate the effects of a finite volume extension for nucleons immersed in nuclear matter. We wish in this way to explore the role played by this non-vanishing (but fixed) volume in shaping nuclear matter properties, in contrast with other models of nuclear physics in which nucleons are treated as point-like particles. We introduce a model characterized by an exclusion volume à la Van der Waals, as well as an effective non-relativistic approximation to model meson-exchange interactions between nucleons. The model is consistent with experimental values of saturation density and binding energy of nuclear matter in the domain of typical densities for neutron stars.

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