scholarly journals Relativistic mean-field corrections for interactions of dark matter particles with nucleons

2021 ◽  
Vol 103 (3) ◽  
Author(s):  
X. G. Wang ◽  
A. W. Thomas
Keyword(s):  
Dark Matter ◽  
Mean Field ◽  
Relativistic Mean Field

scholarly journals Effects of dark matter on the nuclear and neutron star matter

2020 ◽  
Vol 495 (4) ◽  
pp. 4893-4903 ◽  
Author(s):  
H C Das ◽  
Ankit Kumar ◽  
Bharat Kumar ◽  
S K Biswal ◽  
Takashi Nakatsukasa ◽  
...  
Keyword(s):  
Dark Matter ◽  
Neutron Star ◽  
Symmetry Energy ◽  
Mean Field ◽  
Mean Field Model ◽  
Relativistic Mean Field ◽  
Equation Of States ◽  
Astrophysical Objects ◽  
Pure Neutron Matter ◽  
The Moment

ABSTRACT We study the dark matter (DM) effects on the nuclear matter (NM) parameters characterizing the equation of states of super dense neutron-rich nucleonic matter. The observables of the NM, i.e. incompressibility, symmetry energy and its higher order derivatives in the presence DM for symmetric and asymmetric NM are analysed with the help of an extended relativistic mean field model. The calculations are also extended to β-stable matter to explore the properties of the neutron star (NS). We analyse the DM effects on symmetric NM, pure neutron matter, and NS using NL3, G3, and IOPB-I forces. The binding energy per particle and pressure is calculated with and without considering the DM interaction with the NM systems. The influences of DM are also analysed on the symmetry energy and its different coefficients. The incompressibility and the skewness parameters are affected considerably due to the presence of DM in the NM medium. We extend the calculations to the NS and find its mass, radius and the moment of inertia for static and rotating NS with and without DM contribution. The mass of the rotating NS is considerably changing due to rapid rotation with the frequency in the mass-shedding limit. The effects of DM are found to be important for some of the NM parameters, which are crucial for the properties of astrophysical objects.

scholarly journals Effects of dark matter on the in-spiral properties of the binary neutron stars

2021 ◽  
Vol 507 (3) ◽  
pp. 4053-4060
Author(s):  
H C Das ◽  
Ankit Kumar ◽  
S K Patra
Keyword(s):  
Dark Matter ◽  
Neutron Star ◽  
Mean Field ◽  
Time Duration ◽  
Mean Field Model ◽  
Binary Neutron Star ◽  
Relativistic Mean Field ◽  
Orbital Phase ◽  
High Fraction ◽  
Spiral Phase

ABSTRACT Using the relativistic mean-field model, we calculate the properties of binary neutron star (BNS) in the in-spiral phase. Assuming the dark matter (DM) particles are accreted inside the neutron star (NS) due to its enormous gravitational field, the mass M, radius R, tidal deformability λ, and dimensionless tidal deformability Λ are calculated at different DM fractions. The value of M, R, λ, and Λ decreases with the increase of DM percentage inside the NS. The in-spiral phase properties of the BNS are explored within the post-Newtonian (PN) formalism, as it is suitable up to the last orbits in the in-spiral phase. We calculate the strain amplitude of the polarization waveform h+ and h×, (2,2) mode waveform h22, orbital phase Φ, frequency of the gravitational wave f, and PN parameter x with DM as an extra candidate inside the NS. The magnitude of f, Φ, and x are almost the same for all assumed forces; however, the in-spiral time duration in the last orbit is different. We find that the BNS with soft equation of state and a high fraction of DM sustains more time in their in-spiral phase. We suggest that one should take DM inside the NS when they modelling the in-spiral waveforms for the BNS systems.

EVOLUTION OF SHELL STRUCTURE IN NUCLEI

2011 ◽  
Vol 20 (08) ◽  
pp. 1663-1675 ◽  
Author(s):  
A. BHAGWAT ◽  
Y. K. GAMBHIR
Keyword(s):  
Shell Structure ◽  
Crucial Role ◽  
Field Model ◽  
Mean Field ◽  
Mass Region ◽  
The Other ◽  
Mean Field Model ◽  
Relativistic Mean Field ◽  
Shell Closures ◽  
Low Mass

Systematic investigations of the pairing and two-neutron separation energies which play a crucial role in the evolution of shell structure in nuclei, are carried out within the framework of relativistic mean-field model. The shell closures are found to be robust, as expected, up to the lead region. New shell closures appear in low mass region. In the superheavy region, on the other hand, it is found that the shell closures are not as robust, and they depend on the particular combinations of neutron and proton numbers. Effect of deformation on the shell structure is found to be marginal.

TABLE OF GROUND STATE PROPERTIES OF NUCLEI IN THE RMF MODEL

2013 ◽  
Vol 28 (16) ◽  
pp. 1350068 ◽  
Author(s):  
TUNCAY BAYRAM ◽  
A. HAKAN YILMAZ
Keyword(s):  
Ground State ◽  
Mean Field ◽  
Properties Of Nuclei ◽  
Relativistic Mean Field ◽  
Ground State Properties ◽  
Pairing Correlations ◽  
Ground State Energies ◽  
Rmf Model

The ground state energies, sizes and deformations of 1897 even–even nuclei with 10≤Z ≤110 have been carried out by using the Relativistic Mean Field (RMF) model. In the present calculations, the nonlinear RMF force NL3* recent refitted version of the NL3 force has been used. The BCS (Bardeen–Cooper–Schrieffer) formalism with constant gap approximation has been taken into account for pairing correlations. The predictions of RMF model for the ground state properties of some nuclei have been discussed in detail.

Relativistic mean field description of Zn and Ge nuclei

1999 ◽  
Vol 59 (5) ◽  
pp. 2541-2545 ◽  
Author(s):  
G. Gangopadhyay
Keyword(s):  
Mean Field ◽  
Relativistic Mean Field
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