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NSR database version of May 24, 2024.

Search: Author = C.Mondal

Found 18 matches.

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2023MO03      Phys.Rev. C 107, 015801 (2023)

C.Mondal, F.Gulminelli

Nucleonic metamodeling in light of multimessenger, PREX-II, and CREX data

NUCLEAR STRUCTURE 48Ca, 208Pb; calculated posterior probability distributions of binding energies, neutron skin thickness, symmetry energy parameters. Full Bayesian study for static astrophysical observables as well as ground-state finite nuclear properties. Nuclear metamodelling technique used to calculate the ground-state properties of nuclei within the extended Thomas-Fermi (ETF) method.

doi: 10.1103/PhysRevC.107.015801
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2023TH01      Phys.Rev. C 107, 015803 (2023)

V.Thakur, R.Kumar, P.Kumar, M.Kumar, C.Mondal, K.Huang, J.Hu, B.K.Agrawal, S.K.Dhiman

Relativistic approach for the determination of nuclear and neutron star properties in consideration of PREX-II results

NUCLEAR STRUCTURE A=20-220; calculated charge rms radii, binding energy. 48Ca, 208Pb; calculated neutron skin thickness. Obtained properties of nonrotating neutron star. New parametrization of the relativistic mean-field (RMF) model obtained by fit to the available experimental data on binding energy, charge rms radii and taking into account recent PREX-II results on neutron skin thickness. Comparison to results obtained with different parametrizations - NL3, IOPB-I, FSUGarnet, Big Apple.

doi: 10.1103/PhysRevC.107.015803
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2022AD03      Phys.Rev. C 105, 015806 (2022)

S.M.Adil Imam, N.K.Patra, C.Mondal, T.Malik, B.K.Agrawal

Bayesian reconstruction of nuclear matter parameters from the equation of state of neutron star matter

doi: 10.1103/PhysRevC.105.015806
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2022MO09      Phys.Rev. C 105, 034305 (2022)

C.Mondal

Density dependence of symmetry energy and neutron skin thickness revisited using relativistic mean field models with nonlinear couplings

NUCLEAR STRUCTURE 16O, 40,48Ca, 56,68Ni, 90Zr, 100,116,132Sn, 144Sm, 208Pb; analyzed binding energies, charge radii, neutron-skin thickness; deduced symmetry energy and density slope parameter as a function of density, correlation coefficient between neutron skin-thickness and density slope parameter. Parameters of the FSU type relativistic models obtained by fitting binding energies and charge radii of the closed-shell spherical nuclei while keeping fixed value of neutron skin-thickness in 208Pb.

doi: 10.1103/PhysRevC.105.034305
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2022TH07      Phys.Rev. C 106, 045806 (2022)

V.Thakur, R.Kumar, P.Kumar, V.Kumar, M.Kumar, C.Mondal, B.K.Agrawal, S.K.Dhiman

Effects of an isovector scalar meson on the equation of state of dense matter within a relativistic mean field model

NUCLEAR STRUCTURE 16,24O, 40,48Ca, 56,78Ni, 88Sr, 90Zr , 100,116,132Sn, 208Pb; analyzed experimental values of binding energy, charge radii, neutron skin thickness; deduced mass-radius relation of a neutron star, variation of dimensionless tidal deformability with respect to gravitational mass. Calculations within relativistic mean field (RMF) framework withadded freedom in the isospin channel through the δ meson.

doi: 10.1103/PhysRevC.106.045806
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2021AH05      Nucl.Phys. A1016, 122334 (2021)

M.Ahmady, D.Chakrabarti, C.Mondal, R.Sandapen

Nucleon electroweak form factors using spin-improved holographic light-front wavefunctions

doi: 10.1016/j.nuclphysa.2021.122334
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2021DU08      Phys.Rev. C 103, 035202 (2021)

M.Dutra, O.Lourenco, X.Vinas, C.Mondal

Analysis of critical parameters for nonrelativistic models of symmetric nuclear matter

doi: 10.1103/PhysRevC.103.035202
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2020MO26      Phys.Rev. C 102, 015802 (2020)

C.Mondal, X.Vinas, M.Centelles, J.N.De

Structure and composition of the inner crust of neutron stars from Gogny interactions

NUCLEAR STRUCTURE A=15-215; calculated binding energies using variational Wigner-Kirkwood with shell and pairing corrections (VWKSP) and HFB methods using D1M, D1S and D1M* Gogny forces, and compared to experimental values for about 160 even-even nuclei. Z=5-100; calculated binding energies per particle at different nucleon densities for inner crust of neutron star subtracted by free nucleon mass using the D1M* Gogny force. 32Mg, 40,50Ca, 90Zr, 100Sn, 142Sm, 176Hg, 208Pb, 216Po, 224U; calculated binding energies using VWKSP and HFB methods using D1M* Gogny force and compared with experimental values. Calculated number of protons (Z=20-92) and the total number of baryons (A=100-2500) corresponding to the β-equilibrium configurations as a function of the inner crust density, and constructed the equation of state (EoS) of the inner crust of neutron stars for D1M, D1S and D1M* interactions.

doi: 10.1103/PhysRevC.102.015802
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2019MA35      Phys.Rev. C 99, 052801 (2019)

T.Malik, B.K.Agrawal, J.N.De, S.K.Samaddar, C.Providencia, C.Mondal, T.K.Jha

Tides in merging neutron stars: Consistency of the GW170817 event with experimental data on finite nuclei

doi: 10.1103/PhysRevC.99.052801
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2018MA70      Phys.Rev. C 98, 064316 (2018)

T.Malik, C.Mondal, B.K.Agrawal, J.N.De, S.K.Samaddar

Nucleon effective mass and its isovector splitting

NUCLEAR STRUCTURE 48Ca, 68Ni, 120Sn, 208Pb; calculated dipole enhancement factor, correlation of the isovector parameter, and energy weighted sum rule using energy density functional (EDF) based on the thermodynamic Gibbs-Duhem relation. Nucleon effective mass and its isovector splitting. Comparison with other theoretical predictions.

doi: 10.1103/PhysRevC.98.064316
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2018MO26      Int.J.Mod.Phys. E27, 1850078 (2018)

C.Mondal, B.K.Agrawal, J.N.De, S.K.Samaddar

Correlations among symmetry energy elements in Skyrme models

doi: 10.1142/S0218301318500787
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2017KU31      Eur.Phys.J. A 53, 237 (2017)

N.Kumar, C.Mondal, N.Sharma

Gravitational form factors and angular momentum densities in light-front quark-diquark model

doi: 10.1140/epja/i2017-12433-0
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2017MO16      Eur.Phys.J. A 53, 106 (2017)

C.Mondal, D.Chakrabarti, X.Zhao

Deuteron transverse densities in holographic QCD

doi: 10.1140/epja/i2017-12292-7
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2017MO23      Phys.Rev. C 96, 021302 (2017)

C.Mondal, B.K.Agrawal, J.N.De, S.K.Samaddar, M.Centelles, X.Vinas

Interdependence of different symmetry energy elements

doi: 10.1103/PhysRevC.96.021302
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2016CH43      Eur.Phys.J. A 52, 285 (2016)

D.Chakrabarti, C.Mondal

Nucleon-to-Δ transition form factors and empirical transverse charge densities

doi: 10.1140/epja/i2016-16285-8
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2016MO10      Phys.Rev. C 93, 044328 (2016)

C.Mondal, B.K.Agrawal, J.N.De, S.K.Samaddar

Sensitivity of elements of the symmetry energy of nuclear matter to the properties of neutron-rich systems

NUCLEAR STRUCTURE 16,24O, 20,30Ne, 24,36Mg, 40,48,54,58Ca, 56,68,78Ni, 90Zr, 100,116,132,138Sn, 144Sm, 208Pb; analyzed best-fit parameters for binding energy and charge radius of a nucleus. Nuclear symmetry energy matter density for ultra-neutron-rich nuclei. Maximum mass of a neutron star. Relativistic mean field model.

doi: 10.1103/PhysRevC.93.044328
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2016MO20      Phys.Rev. C 93, 064303 (2016)

C.Mondal, B.K.Agrawal, M.Centelles, G.Colo, X.Roca-Maza, N.Paar, X.Vinas, S.K.Singh, S.K.Patra

Model dependence of the neutron-skin thickness on the symmetry energy

NUCLEAR STRUCTURE 132Sn, 208Pb; calculated symmetry-energy coefficient and symmetry-energy slope parameter as a function of neutron-skin thickness using several microscopic mean-field models.

doi: 10.1103/PhysRevC.93.064303
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2015MO16      Phys.Rev. C 92, 024302 (2015)

C.Mondal, B.K.Agrawal, J.N.De

Constraining the symmetry energy content of nuclear matter from nuclear masses: A covariance analysis

NUCLEAR STRUCTURE 16,24O, 18,30Ne, 40,48Ca, 56,68Ni, 90Zr, 100,116,132Sn, 144Sm, 208Pb; calculated binding energies and charge radii, binding energy/nucleon, incompressibility coefficient K, Dirac effective mass of nucleon, symmetry energy coefficient, density slope parameter of symmetry energy, and neutron skins using two different models and constrained by experimental masses. Covariance analysis. Relativistic mean-field (RMF) approach using 16 different models.

doi: 10.1103/PhysRevC.92.024302
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