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NSR database version of April 11, 2024.

Search: Author = F.J.Fattoyev

Found 28 matches.

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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
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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
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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
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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
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2019PI07      Phys.Rev. C 99, 045802 (2019)

J.Piekarewicz, F.J.Fattoyev

Impact of the neutron star crust on the tidal polarizability

doi: 10.1103/PhysRevC.99.045802
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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2013FA09      Phys.Rev.Lett. 111, 162501 (2013)

F.J.Fattoyev, J.Piekarewicz

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
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2012FA05      Phys.Rev. C 86, 015802 (2012)

F.J.Fattoyev, J.Piekarewicz

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
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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
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2011FA12      Phys.Rev. C 84, 064302 (2011)

F.J.Fattoyev, J.Piekarewicz

Accurate calibration of relativistic mean-field models: Correlating observables and providing meaningful theoretical uncertainties

doi: 10.1103/PhysRevC.84.064302
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2010FA11      Phys.Rev. C 82, 025805 (2010)

F.J.Fattoyev, J.Piekarewicz

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
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2010FA12      Phys.Rev. C 82, 025810 (2010)

F.J.Fattoyev, J.Piekarewicz

Sensitivity of the moment of inertia of neutron stars to the equation of state of neutron-rich matter

doi: 10.1103/PhysRevC.82.025810
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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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