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NSR database version of April 27, 2024.

Search: Author = B.K.Sharma

Found 20 matches.

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2024TH01      Phys.Rev. C 109, 025805 (2024)

P.Thakur, B.K.Sharma, A.Ashika, S.Srivishnu, T.K.Jha

Influence of the symmetry energy and σ-cut potential on the properties of pure nucleonic and hyperon-rich neutron star matter

doi: 10.1103/PhysRevC.109.025805
Citations: PlumX Metrics

2023JE03      Acta Phys.Pol. A143, 4-A1 (2023)

K.K.Jena, B.Sahu, J.K.Nayak, P.R.Preethi, B.K.Sharma, S.K.Agarwalla

Simultaneous Study of Scattering and Fusion Hindrance Near Coulomb Barrier in F+Pb Systems

NUCLEAR REACTIONS 208Pb(19F, 19F), (19F, X), E(cm)=80.6-94 MeV; analyzed available data; deduced energy-dependent parameters of the optical potential, fusion σ. The paradigm of the Ginocchio potential.

doi: 10.5506/APhysPolB.54.4-A1
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2022PA35      Phys.Rev. C 106, 055806 (2022)

N.K.Patra, B.K.Sharma, A.Reghunath, A.K.H.Das, T.K.Jha

Effect of the σ-cut potential on the properties of neutron stars with or without a hyperonic core

doi: 10.1103/PhysRevC.106.055806
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2020SH23      Nucl.Phys. A1002, 121974 (2020)

B.K.Sharma, S.Sathees, M.K.Meghaa, T.K.Jha

Effect of Λμ coupling on liquid gas phase transition in warm asymmetric nuclear matter

doi: 10.1016/j.nuclphysa.2020.121974
Citations: PlumX Metrics

2010CE01      J.Phys.(London) G37, 075107 (2010)

M.Centelles, S.K.Patra, X.Roca-Maza, B.K.Sharma, P.D.Stevenson, X.Vinas

The influence of the symmetry energy on the giant monopole resonance of neutron-rich nuclei analyzed in Thomas-Fermi theory

NUCLEAR STRUCTURE 90Zr, 208,266Pb; calculated neutron skin thickness, energy per particle, giant monopole resonance. Relativistic extended Thomas-Fermi method.

doi: 10.1088/0954-3899/37/7/075107
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2010SH11      Phys.Rev. C 81, 064304 (2010)

B.K.Sharma, S.Pal

Nuclear symmetry energy effects on liquid-gas phase transition in hot asymmetric nuclear matter

doi: 10.1103/PhysRevC.81.064304
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2010SH29      Phys.Rev. C 82, 055802 (2010)

B.K.Sharma, S.Pal

Role of isospin physics in supernova matter and neutron stars

doi: 10.1103/PhysRevC.82.055802
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2008GU20      Int.J.Mod.Phys. E17, 2244 (2008)

R.K.Gupta, S.K.Arun, D.Singh, R.Kumar, Niyti, SK.Patra, P.Arumugam, B.K.Sharma

Clusters in light, heavy, super-heavy and super-superheavy nuclei

doi: 10.1142/S0218301308011422
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2007PA30      J.Phys.(London) G34, 2073 (2007)

S.K.Patra, R.K.Gupta, B.K.Sharma, P.D.Stevenson, W.Greiner

Exotic clustering in heavy and superheavy nuclei within the relativistic and non-relativistic mean field formalisms

NUCLEAR STRUCTURE 222Ra, 232U, 236Pu, 242Cm; Z=114; calculated binding energies, deformation parameters, and rms charge radii within the relativistic mean field approach and the non-relativistic Skyrme-Hartree-Fock formalism.

doi: 10.1088/0954-3899/34/9/016
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2007SH13      Phys.Rev. C 75, 035808 (2007)

B.K.Sharma, P.K.Panda, S.K.Patra

Phase transition and properties of a compact star

doi: 10.1103/PhysRevC.75.035808
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2007SH33      Phys.Rev. C 76, 034601 (2007)

A.Shukla, B.K.Sharma, R.Chandra, P.Arumugam, S.K.Patra

Nuclear reaction studies of unstable nuclei using relativistic mean field formalisms in conjunction with the Glauber model

NUCLEAR REACTIONS 12C(12C, X), E < 1000 MeV/nucleon; 12C(Li, X), (Be, X), (B, X)E=800 MeV/nucleon; 12C(11Li, X), (14Be, X), (11Be, X), E=30, 85 MeV/nucleon; calculated σ, angular distributions and total reaction cross sections within the Glauber model. Compared results to available data.

doi: 10.1103/PhysRevC.76.034601
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2006ME12      Int.J.Mod.Phys. E15, 1149 (2006)

M.S.Mehta, B.K.Sharma, S.K.Patra, R.K.Gupta, W.Greiner

Decrease of the spin-orbit interaction in drip-line nuclei, using relativistic mean field models

NUCLEAR STRUCTURE F, Mg, Sb, Pb, Bi; calculated spin-orbit splitting energy vs neutron excess. 120,130,140,150,160,170,180,190Nd; calculated radial dependence of spin-orbit potential.

doi: 10.1142/S0218301306004740
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2006SH01      J.Phys.(London) G32, L1 (2006)

B.K.Sharma, P.Arumugam, S.K.Patra, P.D.Stevenson, R.K.Gupta, W.Greiner

Clustering in superheavy nuclei within the relativistic mean field approach

NUCLEAR STRUCTURE 292,296,300,304120; calculated binding energies, deformation parameters, radii, matter density distributions; deduced cluster configurations. Relativistic mean field approach.

doi: 10.1088/0954-3899/32/1/L01
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2006SH20      J.Phys.(London) G32, 2089 (2006)

B.K.Sharma, S.K.Patra, R.K.Gupta, A.Shukla, P.Arumugam, P.D.Stevenson, W.Greiner

Reaction cross-sections for light nuclei on 12C using relativistic mean field formalism

NUCLEAR REACTIONS 12C(8B, X), (9B, X), (10B, X), (11B, X), (12B, X), (13B, X), (14B, X), (15B, X), (16B, X), (17B, X), (18B, X), (19B, X), (7Be, X), (8Be, X), (9Be, X), (10Be, X), (11Be, X), (12Be, X), (13Be, X), (14Be, X), (6Li, X), (7Li, X), (8Li, X), (9Li, X), (10Li, X), (11Li, X), E ≈ 800 MeV/nucleon; calculated reaction σ. Relativistic mean field approach.

NUCLEAR STRUCTURE 6,7,8,9,10,11Li, 10,11,12,13,14Be, 15,16,17B; calculated binding energies, deformation. Relativistic mean field approach.

doi: 10.1088/0954-3899/32/11/004
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2005AR12      Phys.Rev. C 71, 064308 (2005)

P.Arumugam, B.K.Sharma, S.K.Patra, R.J.K.Gupta

Relativistic mean field study of clustering in light nuclei

NUCLEAR STRUCTURE 16O, 32S; calculated binding energies, rms radii, matter density distributions, deformation parameters. 6,7,8,9,10,11,12,13,14Be, 11,13,15,17,19B; calculated binding energies, deformation parameters, neutron and proton density distributions. 12C, 20Ne, 24Mg, 28Si; calculated binding energies, matter density distributions, deformation parameters. Comparison with data, relativistic mean field approach.

doi: 10.1103/PhysRevC.71.064308
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2004AR23      Phys.Lett. B 601, 51 (2004)

P.Arumugam, B.K.Sharma, P.K.Sahu, S.K.Patra, T.Sil, M.Centelles, X.Vinas

Versatility of field theory motivated nuclear effective Lagrangian approach

doi: 10.1016/j.physletb.2004.09.026
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2004NA22      Pramana 62, 827 (2004)

Z.Naik, B.K.Sharma, T.K.Jha, P.Arumugam, S.K.Patra

Shape change in Hf, W and Os-isotopes: A non-relativistic Hartree-Fock versus relativistic Hartree approximation

NUCLEAR STRUCTURE Hf, W, Os; calculated binding energies, quadrupole deformation parameters. Comparison of relativistic and nonrelativistic approaches.

doi: 10.1007/BF02706132
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2004SH43      Phys.Rev. C 70, 044606 (2004)

M.K.Sharma, Unnati, B.K.Sharma, B.P.Singh, H.D.Bhardwaj, R.Kumar, K.S.Golda, R.Prasad

Complete and incomplete fusion reactions in the 16O + 169Tm system: Excitation functions and recoil range distributions

NUCLEAR REACTIONS 169Tm(16O, 3n), (16O, 4n), (16O, 2np), (16O, 3np), (16O, 2n2p), (16O, 3nα), (16O, np2α), (16O, nα), E=71-95 MeV; measured excitation functions, recoil range distributions. Activation technique, comparison with model predictions.

doi: 10.1103/PhysRevC.70.044606
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Data from this article have been entered in the EXFOR database. For more information, access X4 datasetD6038.

2004SI13      Phys.Rev. C 69, 044315 (2004)

T.Sil, S.K.Patra, B.K.Sharma, M.Centelles, X.Vinas

Superheavy nuclei in a relativistic effective Lagrangian model

NUCLEAR STRUCTURE Z=120; calculated two-neutron separation energies, pair gaps vs neutron number. Z=100-140; calculated two-proton separation energies, pair gaps for N=172, 184, 258 isotones. 298Fl, 292,304,378120; calculated single-particle level energies. Relativistic effective Lagrangian model, possible shell effects discussed.

doi: 10.1103/PhysRevC.69.044315
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1993SH26      Pramana 40, 399 (1993)

B.K.Sharma, B.L.Ahuja, H.Singh, F.M.Mohammad

Compton Profile of Molybdenum

ATOMIC PHYSICS Mo(γ, γ), E=59.54 keV; measured Compton profile. Polycrystalline molybdenum.

doi: 10.1007/BF02847500
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