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NSR database version of May 24, 2024.

Search: Author = K.Oyamatsu

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2023OY01      Prog.Theor.Exp.Phys. 2023, 063D03 (2023)

K.Oyamatsu

Nuclear masses and the equation of state of nuclear matter

NUCLEAR STRUCTURE A>40; analyzed available data; deduced incompressible liquid-drop (ILD) model volume, surface, symmetry, and Coulomb energies are related to the equation of state of nuclear matter using the Oyamatsu–Iida (OI) macroscopic nuclear model, which has reasonable many-body energy and isoscalar inhomogeneity gradient energy.

doi: 10.1093/ptep/ptad072
Citations: PlumX Metrics


2015SO03      Phys.Rev. C 91, 015805 (2015)

H.Sotani, K.Iida, K.Oyamatsu

Constraining the density dependence of the nuclear symmetry energy from an x-ray bursting neutron star

doi: 10.1103/PhysRevC.91.015805
Citations: PlumX Metrics


2014II01      Eur.Phys.J. A 50, 42 (2014)

K.Iida, K.Oyamatsu

Symmetry energy, unstable nuclei and neutron star crusts

doi: 10.1140/epja/i2014-14042-9
Citations: PlumX Metrics


2011II01      Prog.Theor.Phys.(Kyoto) 126, 1091 (2011)

K.Iida, K.Oyamatsu, B.Abu-Ibrahim, A.Kohama

Proton-Nucleus Total Reaction Cross Sections in the Optical Limit Glauber Theory -Subtle Dependence on the Equation of State of Nuclear Matter -

NUCLEAR REACTIONS 112,124Sn, 80Ni(p, X), E=40, 300, 800 MeV; calculated total σ. Glauber theory.

doi: 10.1143/PTP.126.1091
Citations: PlumX Metrics


2011NA22      Phys.Rev. C 83, 065811 (2011)

K.Nakazato, K.Iida, K.Oyamatsu

Curvature effect on nuclear "pasta": Is it helpful for gyroid appearance?

doi: 10.1103/PhysRevC.83.065811
Citations: PlumX Metrics


2010OY01      Phys.Rev. C 81, 054302 (2010)

K.Oyamatsu, K.Iida

Symmetry energy at subnuclear densities deduced from nuclear masses

NUCLEAR STRUCTURE Z=8, A=11-28; Z=12, A=17-43; Z=20, A=30-72; Z=28, A=45-100; Z=50, A=90-180; Z=82, A=175-285; calculated two proton separation energies, δVnp, influence of the density dependence of the symmetry energy on nuclear masses using a macroscopic nuclear model. Comparison with experimental data.

doi: 10.1103/PhysRevC.81.054302
Citations: PlumX Metrics


2010OY02      Phys.Rev. C 82, 027301 (2010)

K.Oyamatsu, K.Iida, H.Koura

Neutron drip line and the equation of state of nuclear matter

doi: 10.1103/PhysRevC.82.027301
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2009NA19      Phys.Rev.Lett. 103, 132501 (2009)

K.Nakazato, K.Oyamatsu, S.Yamada

Gyroid Phase in Nuclear Pasta

doi: 10.1103/PhysRevLett.103.132501
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2008KO29      Phys.Rev. C 78, 061601 (2008)

A.Kohama, K.Iida, K.Oyamatsu

Difference between interaction cross sections and reaction cross sections

NUCLEAR REACTIONS 12C(3He, X), (α, X), (6Li, X), (7Li, X), (9Be, X), (10B, X), (11B, X), (12C, X), (13C, X), (14N, X), (15N, X), (16O, X), (17O, X), (18O, X), (19F, X), (20Ne, X), (21Ne, X), (23Na, X), (24Mg, X), (25Mg, X), (27Al, X), (35Cl, X), (37Cl, X), (36Ar, X), (38Ar, X), (40Ar, X), (80Kr, X), E>800 MeV; calculated reaction σ. Comparisons with data.

doi: 10.1103/PhysRevC.78.061601
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2007KA48      Nucl.Phys. A791, 232 (2007)

H.Kanzawa, K.Oyamatsu, K.Sumiyoshi, M.Takano

Variational calculation for the equation of state of nuclear matter at finite temperatures

doi: 10.1016/j.nuclphysa.2007.01.098
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2007OY01      Phys.Rev. C 75, 015801 (2007)

K.Oyamatsu, K.Iida

Symmetry energy at subnuclear densities and nuclei in neutron star crusts

doi: 10.1103/PhysRevC.75.015801
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2005KO28      Phys.Rev. C 72, 024602 (2005)

A.Kohama, K.Iida, K.Oyamatsu

Reaction cross section described by a black sphere approximation of nuclei

NUCLEAR REACTIONS 4He, 12,13C, 14N, 16O, 20,22Ne, 24,26Mg, 28Si, 32,34S, 39K, 40,42,44,48Ca, 46,48Ti, 120Sn, 208Pb(p, p), E ≈ 800-1100 MeV; analyzed σ(θ); deduced black-sphere radius parameters. 12C, 120Sn, 208Pb(p, X), E ≈ 800 MeV; analyzed reaction, interaction σ.

doi: 10.1103/PhysRevC.72.024602
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2004II01      Phys.Rev. C 69, 037301 (2004)

K.Iida, K.Oyamatsu

Surface tension in a compressible liquid-drop model: Effects on nuclear density and neutron skin thickness

NUCLEAR STRUCTURE 56,64Ni, 90Zr, 116,124Sn, 208Pb; calculated neutron and proton radii, role of surface tension. Compressible liquid-drop model.

doi: 10.1103/PhysRevC.69.037301
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2004II02      Prog.Theor.Phys.(Kyoto), Suppl. 156, 139 (2004)

K.Iida, K.Oyamatsu, B.Abu-Ibrahim

Deducing the Density Dependence of the Symmetry Energy from Unstable Nuclei

NUCLEAR REACTIONS 58Ni(p, p), E=400, 1047 MeV; 58,80Ni, 124Sn, 208Pb(p, p), E=800 MeV; calculated σ(θ), density dependence features. Glauber model.

doi: 10.1143/PTPS.156.139
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2004KO34      Phys.Rev. C 69, 064316 (2004)

A.Kohama, K.Iida, K.Oyamatsu

Nuclear radius deduced from proton diffraction by a black nucleus

NUCLEAR REACTIONS 58,60,62,64Ni(p, p), E ≈ 800-1050 MeV; 90,92Zr, 120Sn, 144,154Sm, 176Yb, 208Pb(p, p), E=800 MeV; analyzed σ(θ); deduced radii. Black-sphere approach.

doi: 10.1103/PhysRevC.69.064316
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2004OY01      Prog.Theor.Phys.(Kyoto), Suppl. 156, 137 (2004)

K.Oyamatsu, K.Iida

Equation of State of Nuclear Matter, Neutron Rich Nuclei in Laboratories and Pasta Nuclei in Neutron Star Crusts

NUCLEAR STRUCTURE 80Ni; calculated matter radius.

doi: 10.1143/PTPS.156.137
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2003II02      Phys.Lett. B 576, 273 (2003)

K.Iida, K.Oyamatsu, B.Abu-Ibrahim

Proton-nucleus elastic scattering and the equation of state of nuclear matter

NUCLEAR REACTIONS 58Ni(p, p), E=400, 1047 MeV; 58,80Ni, 116,124Sn, 208Pb(p, p), E=800 MeV; calculated σ(θ); deduced dependence on nuclear matter density parameter. Glauber model.

doi: 10.1016/j.physletb.2003.10.019
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2003OY01      Nucl.Phys. A718, 363c (2003)

K.Oyamatsu, K.Iida

Empirical properties of asymmetric nuclear matter to be obtained from unstable nuclei

NUCLEAR STRUCTURE 80Ni; calculated matter radius vs density symmetry coefficient. Ni; calculated matter radii for N=18-64.

doi: 10.1016/S0375-9474(03)00740-1
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2003OY02      Prog.Theor.Phys.(Kyoto) 109, 631 (2003)

K.Oyamatsu, K.Iida

Saturation of Nuclear Matter and Radii of Unstable Nuclei

NUCLEAR STRUCTURE 90Zr, 208Pb; calculated matter density distributions. 58,80Ni, 116,142Sn; calculated radii, parameter dependences, saturation properties.

doi: 10.1143/PTP.109.631
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2003SH33      Nucl.Phys. A721, 1048c (2003)

H.Shen, H.Toki, K.Oyamatsu, K.Sumiyoshi

Relativistic equation of state for supernova and neutron star

doi: 10.1016/S0375-9474(03)01282-X
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2002OY01      J.Nucl.Sci.Technol.(Tokyo) 39, 337 (2002)

K.Oyamatsu

Exploring Neutron-Star Matter using RI Beam

NUCLEAR STRUCTURE Sn; calculated radii for two equations of state. Investigation of neutron-rich nuclides with radioactive beams discussed.

doi: 10.1080/18811248.2002.9715199
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2002OY02      Prog.Theor.Phys.(Kyoto), Suppl. 146, 613 (2002)

K.Oyamatsu

A Criterion to Obtain the Equation of State of Asymmetric Nuclear Matter

doi: 10.1143/PTPS.146.613
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2001KA46      J.Nucl.Sci.Technol.(Tokyo) 38, 470 (2001)

J.-I.Katakura, T.Yoshida, K.Oyamatsu, T.Tachibana

Estimation of Beta- and Gamma-Ray Spectra for JENDL FP Decay Data File

RADIOACTIVITY 99Sr, 143,144Cs(β-); calculated Eβ, Eγ. Fission product nuclei, gross theory of beta decay.

NUCLEAR REACTIONS 241Pu(n, F), E=thermal; calculated aggregate fission product Eβ, Eγ. Comparison with data.

doi: 10.1080/18811248.2001.9715056
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2001OY01      J.Nucl.Sci.Technol.(Tokyo) 38, 477 (2001)

K.Oyamatsu, H.Takeuchi, M.Sagisaka, J.-i.Katakura

New Method for Calculating Aggregate Fission Product Decay Heat with Full Use of Macroscopic-Measurement Data

NUCLEAR REACTIONS 232Th(n, F)137Cs/86Se/87Se/102Zr, E fast; 233U(n, F)88Kr/93Sr/89Kr/100Zr/92Sr, E fast; 235U(n, F)133Te/134Te/100Zr/132Te/96Sr, E fast; 238U(n, F)103Zr/102Zr/100Y, 135Te/136Te, E fast; 239Pu(n, F)104Mo/103Mo, E fast; 235U(n, F)144Ba/133Te/92Sr/140Cs/134Te/100Zr, E thermal; 239Pu(n, F)132Sb/132Te/140Ba/136Xe, E thermal; 241Pu(n, F)108Tc/106Mo/107Mo/138Xe, E thermal; calculated decay heat.

doi: 10.1080/18811248.2001.9715057
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1999MB10      Nucl.Phys. (Supplement) A654, 908c (1999)

T.Maruyama, K.Niita, K.Oyamatsu, T.Maruyama, S.Chiba, A.Iwamoto

Nuclear Matter Structure Studied with Quantum Molecular Dynamics

doi: 10.1016/S0375-9474(00)88570-X
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1998MA04      Phys.Rev. C57, 655 (1998)

T.Maruyama, K.Niita, K.Oyamatsu, T.Maruyama, S.Chiba, A.Iwamoto

Quantum Molecular Dynamics Approach to the Nuclear Matter Below the Saturation Density

doi: 10.1103/PhysRevC.57.655
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1998OY01      Nucl.Phys. A634, 3 (1998)

K.Oyamatsu, I.Tanihata, Y.Sugahara, K.Sumiyoshi, H.Toki

Can the Equation of State of Asymmetric Nuclear Matter be Studied using Unstable Nuclei ( Question )

NUCLEAR STRUCTURE Z=10-90; calculated densities, neutron skin thickness. Sn; calculated neutron, proton diffuseness. 208,266Pb; calculated neutron, proton radial distributions. Comparison of parameter sets. Implications for asymmetric nuclear matter.

doi: 10.1016/S0375-9474(98)00125-0
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1998SH24      Nucl.Phys. A637, 435 (1998)

H.Shen, H.Toki, K.Oyamatsu, K.Sumiyoshi

Relativistic Equation of State of Nuclear Matter for Supernova and Neutron Star

doi: 10.1016/S0375-9474(98)00236-X
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1998SH39      Prog.Theor.Phys.(Kyoto) 100, 1013 (1998)

H.Shen, H.Toki, K.Oyamatsu, K.Sumiyoshi

Relativistic Equation of State of Nuclear Matter for Supernova Explosion

doi: 10.1143/PTP.100.1013
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1995SU16      Nucl.Phys. A595, 327 (1995)

K.Sumiyoshi, K.Oyamatsu, H.Toki

Neutron Star Profiles in the Relativistic Brueckner-Hartree-Fock Theory

doi: 10.1016/0375-9474(95)00388-5
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1994OY01      Nucl.Phys. A578, 181 (1994)

K.Oyamatsu, M.Yamada

Shell Energies of Non-Spherical Nuclei in the Inner Crust of a Neutron Star

NUCLEAR STRUCTURE Z=20-90; N=20-140; calculated crude shell energies. Thomas-Fermi calculations, spherical, non-spherical single particle potentials, neutron star inner crust relevance.

doi: 10.1016/0375-9474(94)90975-X
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1993OY01      Nucl.Phys. A561, 431 (1993)

K.Oyamatsu

Nuclear Shapes in the Inner Crust of a Neutron Star

NUCLEAR STRUCTURE A=25-245; calculated proton number, mass excess, rms radii. 90Zr, 208Pb; calculated charge distributions. Neutron star inner crust nuclear shapes relevance.

doi: 10.1016/0375-9474(93)90020-X
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