NSR Query Results
Output year order : Descending NSR database version of April 27, 2024. Search: Author = F.J.Fattoyev Found 28 matches. 2024RE05 Phys.Rev. C 109, 035803 (2024) B.T.Reed, F.J.Fattoyev, C.J.Horowitz, J.Piekarewicz Density dependence of the symmetry energy in the post-PREX-CREX era
doi: 10.1103/PhysRevC.109.035803
2021RE05 Phys.Rev.Lett. 126, 172503 (2021) B.T.Reed, F.J.Fattoyev, C.J.Horowitz, J.Piekarewicz Implications of PREX-2 on the Equation of State of Neutron-Rich Matter NUCLEAR STRUCTURE 208Pb; analyzed available data for the neutron skin thickness; deduced the slope of the symmetry energy, the impact of stiff symmetry energy on some critical neutron-star observables.
doi: 10.1103/PhysRevLett.126.172503
2020FA09 Phys.Rev. C 102, 065805 (2020) F.J.Fattoyev, C.J.Horowitz, J.Piekarewicz, B.Reed GW190814: Impact of a 2.6 solar mass neutron star on the nucleonic equations of state
doi: 10.1103/PhysRevC.102.065805
2020TS01 Phys.Rev. C 102, 045808 (2020) C.Y.Tsang, M.B.Tsang, P.Danielewicz, W.G.Lynch, F.J.Fattoyev Impact of the neutron-star deformability on equation of state parameters
doi: 10.1103/PhysRevC.102.045808
2019PI07 Phys.Rev. C 99, 045802 (2019) Impact of the neutron star crust on the tidal polarizability
doi: 10.1103/PhysRevC.99.045802
2019TS08 Phys.Rev. C 100, 062801 (2019) C.Y.Tsang, B.A.Brown, F.J.Fattoyev, W.G.Lynch, M.B.Tsang Constraints on Skyrme equations of state from doubly magic nuclei, ab initio calculations of low-density neutron matter, and neutron stars
doi: 10.1103/PhysRevC.100.062801
2018BR08 Phys.Rev.Lett. 120, 182701 (2018) E.F.Brown, A.Cumming, F.J.Fattoyev, C.J.Horowitz, D.Page, S.Reddy Rapid Neutrino Cooling in the Neutron Star MXB 1659-29
doi: 10.1103/PhysRevLett.120.182701
2018FA05 Phys.Rev.Lett. 120, 172702 (2018) F.J.Fattoyev, J.Piekarewicz, C.J.Horowitz Neutron Skins and Neutron Stars in the Multimessenger Era NUCLEAR STRUCTURE 208Pb; calculated neutron star dimensionless tidal polarizability as a function of the neutron-skin thickness of 208Pb, mass-vs-radius relations.
doi: 10.1103/PhysRevLett.120.172702
2018FA08 Phys.Rev. C 98, 025801 (2018) F.J.Fattoyev, E.F.Brown, A.Cumming, A.Deibel, C.J.Horowitz, B.-A.Li, Z.Lin Deep crustal heating by neutrinos from the surface of accreting neutron stars NUCLEAR REACTIONS 1H, Fe(p, π+), Fe(α, π+), E=290-550 MeV/nucleon; calculated multiplicity of pion production as a function of beam energy, total energy per accreted nucleon deposited by neutrinos in the inner crust for a neutron star using the four equations of state, total energy deposited by neutrinos into the inner crust; investigated a new mechanism of deep crustal heating of neutron stars in mass-transferring binaries by neutrinos from decay of charged pions produced at the surface of the neutron stars through p+p, p+Fe and α+Fe collisions.
doi: 10.1103/PhysRevC.98.025801
2017CU02 Phys.Rev. C 95, 025806 (2017) A.Cumming, E.F.Brown, F.J.Fattoyev, C.J.Horowitz, D.Page, S.Reddy Lower limit on the heat capacity of the neutron star core
doi: 10.1103/PhysRevC.95.025806
2017FA05 Phys.Rev. C 95, 055804 (2017) F.J.Fattoyev, C.J.Horowitz, B.Schuetrumpf Quantum nuclear pasta and nuclear symmetry energy
doi: 10.1103/PhysRevC.95.055804
2016SA24 Phys.Rev. C 93, 055801 (2016) I.Sagert, G.I.Fann, F.J.Fattoyev, S.Postnikov, C.J.Horowitz Quantum simulations of nuclei and nuclear pasta with the multiresolution adaptive numerical environment for scientific simulations NUCLEAR STRUCTURE 16O, 208Pb, 238U; calculated nuclear ground states, binding energies, shapes of light and heavy nuclei with different geometries with and without spin-orbit forces via three-dimensional (3D) Skyrme Hartree-Fock (SHF) simulations of nuclear pasta with Multi-resolution ADaptive Numerical Environment for Scientific Simulations (MADNESS); deduced that pasta phase remains in waffle geometry. Relevance to exotic shapes of neutron star and supernova matter.
doi: 10.1103/PhysRevC.93.055801
2015CA14 Phys.Rev. C 92, 015802 (2015) B.-J.Cai, F.J.Fattoyev, B.-A.Li, W.G.Newton Critical density and impact of Δ (1232) resonance formation in neutron stars
doi: 10.1103/PhysRevC.92.015802
2015HE03 Phys.Rev. C 91, 015810 (2015) X.-T.He, F.J.Fattoyev, B.-A.Li, W.G.Newton Impact of the equation-of-state-gravity degeneracy on constraining the nuclear symmetry energy from astrophysical observables
doi: 10.1103/PhysRevC.91.015810
2015JI11 Eur.Phys.J. A 51, 119 (2015) W.-Z.Jiang, B.-A.Li, F.J.Fattoyev Small radii of neutron stars as an indication of novel in-medium effects
doi: 10.1140/epja/i2015-15119-7
2015ST02 Phys.Rev. C 91, 015804 (2015) A.W.Steiner, S.Gandolfi, F.J.Fattoyev, W.G.Newton Using neutron star observations to determine crust thicknesses, moments of inertia, and tidal deformabilities
doi: 10.1103/PhysRevC.91.015804
2014FA05 Eur.Phys.J. A 50, 45 (2014) F.J.Fattoyev, W.G.Newton, B.-A.Li Probing the high-density behavior of symmetry energy with gravitational waves
doi: 10.1140/epja/i2014-14045-6
2014FA12 Phys.Rev. C 90, 022801 (2014) F.J.Fattoyev, W.G.Newton, B.-A.Li Quantifying correlations between isovector observables and the density dependence of the nuclear symmetry energy away from saturation density NUCLEAR STRUCTURE 48Ca, 208Pb; calculated correlations between nuclear symmetry energy S(ρ) and its slope L(ρ), neutron skin thickness, radii of neutron stars, and the crust-core transition pressure for different densities using Skyrme models SLy4 and NRAPR.
doi: 10.1103/PhysRevC.90.022801
2014NE02 Eur.Phys.J. A 50, 41 (2014) W.G.Newton, J.Hooker, M.Gearheart, K.Murphy, D.-H.Wen, F.J.Fattoyev, B.-A.Li Constraints on the symmetry energy from observational probes of the neutron star crust
doi: 10.1140/epja/i2014-14041-x
2014PI06 Phys.Rev. C 90, 015803 (2014) J.Piekarewicz, F.J.Fattoyev, C.J.Horowitz Pulsar glitches: The crust may be enough NUCLEAR STRUCTURE 208Pb; calculated binding energy per nucleon, charge radius, and neutron-skin thickness, fraction of the crustal moment of inertia as a function of the neutron-skin thickness of 208Pb using relativistic mean-field models FSUGold and NL3. Comparison with experimental data. Calculated fractional moment of inertia of neutron stars of various masses using a representative set of relativistic mean-field models.
doi: 10.1103/PhysRevC.90.015803
2013FA02 Phys.Rev. C 87, 015806 (2013) F.J.Fattoyev, J.Carvajal, W.G.Newton, B.-A.Li Constraining the high-density behavior of the nuclear symmetry energy with the tidal polarizability of neutron stars
doi: 10.1103/PhysRevC.87.015806
2013FA09 Phys.Rev.Lett. 111, 162501 (2013) Has a Thick Neutron Skin in 208Pb Been Ruled Out? NUCLEAR STRUCTURE 208Pb; analyzed lead radius experiment data; calculated ground state properties, collective monopole and dipole responses, and mass vs. radius relations for neutron stars. Relativistic models with neutron skin thickness, comparison with available data.
doi: 10.1103/PhysRevLett.111.162501
2012FA05 Phys.Rev. C 86, 015802 (2012) Neutron skins and neutron stars NUCLEAR STRUCTURE 208Pb; calculated mass versus radius of neutron stars, energy per neutron as a function of the Fermi momentum, correlation coefficients between neutron skin thickness of 208Pb and physical observables of relevance to the structure and dynamics of neutron stars using the FSUGold model. Covariance analyses.
doi: 10.1103/PhysRevC.86.015802
2012FA09 Phys.Rev. C 86, 025804 (2012) F.J.Fattoyev, W.G.Newton, J.Xu, B.-A.Li Generic constraints on the relativistic mean-field and Skyrme-Hartree-Fock models from the pure neutron matter equation of state NUCLEAR STRUCTURE 112,114,116,118,120,122,124,126,128,130,132Sn, 208Pb; calculated nuclear symmetry energy, neutron skin thickness. Microscopic pure neutron matter (PNM) calculations using relativistic mean-field (RMF) and Skyrme-Hartree-Fock (SHF) models with IU-FSU and SkIU-FSU parametrizations. 40,48Ca, 78Ni, 90Zr, 132Sn, 208Pb; analyzed relative deviation of the binding energies and charge radii. Comparison with experimental data. Discussed predictions of neutron skin thicknesses and neutron star radii.
doi: 10.1103/PhysRevC.86.025804
2011FA12 Phys.Rev. C 84, 064302 (2011) Accurate calibration of relativistic mean-field models: Correlating observables and providing meaningful theoretical uncertainties
doi: 10.1103/PhysRevC.84.064302
2010FA11 Phys.Rev. C 82, 025805 (2010) Relativistic models of the neutron-star matter equation of state NUCLEAR STRUCTURE 208Pb; calculated binding energy per nucleon, charge radius, neutron thickness using three models (NL3, FSU, XS). Comparison with experimental data. Relativistic equation of state for the neutron-star matter.
doi: 10.1103/PhysRevC.82.025805
2010FA12 Phys.Rev. C 82, 025810 (2010) Sensitivity of the moment of inertia of neutron stars to the equation of state of neutron-rich matter
doi: 10.1103/PhysRevC.82.025810
2010FA18 Phys.Rev. C 82, 055803 (2010) F.J.Fattoyev, C.J.Horowitz, J.Piekarewicz, G.Shen Relativistic effective interaction for nuclei, giant resonances, and neutron stars NUCLEAR STRUCTURE 40,48Ca, 90Zr, 132Sn, 208Pb; calculated binding energy, charge radii, neutron skin thickness, charge and neutron densities, centroid energies of giant-monopole resonances (GMR) using relativistic mean-field (RMF) theory and NL3, FSU and IU-FSU interactions. Equation of state for neutron-star structure. Comparison with experimental data.
doi: 10.1103/PhysRevC.82.055803
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