Eddy current effects in a high field dipole

Zhang, Manzhou; Zhang, Miao; Xie, Xiaoyu; Tan, Songsheng; Zhang, Jidong; Ouyang, Lunqun; Li, Rui; Liu, Deming

doi:10.1007/s41365-017-0325-5

Cited by 10 publications

(8 citation statements)

References 4 publications

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“…For the EOS of SNM, extensive studies have determined the most probable incompressibility of symmetric nuclear matter as K 0 = 230 ± 20 MeV [63,64], while the skewness parameter J 0 is only roughly known to be in the range of −800 ≤ J 0 ≤ 400 MeV [65,66]. For the symmetry energy, past efforts in both nuclear physics and astrophysics have been most fruitful in constraining the magnitude and slope, i.e., E sym (ρ 0 ) and L(ρ 0 ), of the E sym (ρ) around ρ 0 .…”

Section: What Have We Learned About the Symmetry Energy So Far?mentioning

confidence: 99%

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Towards understanding astrophysical effects of nuclear symmetry energy

et al. 2019

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Determining the Equation of State (EOS) of dense neutron-rich nuclear matter is a shared goal of both nuclear physics and astrophysics. Except possible phase transitions, the density dependence of nuclear symmetry Esym(ρ) is the most uncertain part of the EOS of neutron-rich nucleonic matter especially at supra-saturation densities. Much progresses have been made in recent years in predicting the symmetry energy and understanding why it is still very uncertain using various microscopic nuclear many-body theories and phenomenological models. Simultaneously, significant progresses have also been made in probing the symmetry energy in both terrestrial nuclear laboratories and astrophysical observatories. In light of the GW170817 event as well as ongoing or planned nuclear experiments and astrophysical observations probing the EOS of dense neutron-rich matter, we review recent progresses and identify new challenges to the best knowledge we have on several selected topics critical for understanding astrophysical effects of the nuclear symmetry energy.PACS. 2 6.60.Kp Contents B.A Li, P.G. Krastev, D.H. Wen and N.B. Zhang: Astrophysical Effects of Nuclear Symmetry Energy 5.2.2 Predicted correlation strength between the radii of neutron stars and the symmetry energy from low to high densities 32 5.2.3 Predicted effects of the symmetry energy on the tidal deformability of neutron stars 33 5.3 Post-GW170817 analyses of tidal deformability and radii of neutron stars as well as constraints on the nuclear EOS and symmetry energy . . . 34 5.3.

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Section: What Have We Learned About the Symmetry Energy So Far?mentioning

confidence: 99%

“…MeV [66,106,182,271,272]. Within these parameter ranges, the diverse high-density behaviors of E sym (ρ) can be sampled by the parameterization of Eq.…”

Section: Solving the Inverse-structure Problem Of Neutron Stars In A mentioning

confidence: 99%

Towards understanding astrophysical effects of nuclear symmetry energy

et al. 2019

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“…According to the existing knowledge on the parameters near the saturation density of nuclear matter, the most probable values of them are as follows: K 0 = 230 ± 20 MeV, E sym (ρ 0 ) = 31.7 ± 3.2 MeV, L = 58.7 ± 28.1 MeV, and −300 ≤ J 0 ≤ 400 MeV, −400 ≤ K sym ≤ 100 MeV, −200 ≤ J sym ≤ 800 MeV, see, e.g., refs. [34][35][36][37][38][39]. The first three parameters K 0 , E sym (ρ 0 ), and L have already been constrained in their respective narrow ranges, while the last three parameters J 0 , K sym , and J sym still have very large uncertainties.…”

Section: An Explicitly Isospin-dependent Eos For Dense Neutron-rimentioning

confidence: 99%

GW170817 implications on the frequency and damping time of f -mode oscillations of neutron stars

Wang

Chen

et al. 2019

Phys. Rev. C

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Within a minimum model for neutron stars consisting of nucleons, electrons and muons at βequilibrium using about a dozen Equation of States (EOSs) from microscopic nuclear many-body theories and 40,000 EOSs randomly generated using an explicitly isospin-dependent parametric EOS model for high-density neutron-rich nucleonic matter within its currently known uncertainty range, we study correlations among the f-mode frequency, its damping time and the tidal deformability as well as the compactness of neutron stars. Except for quark stars, both the f-mode frequency and damping time of canonical neutron stars are found to scale with the tidal deformability independent of the EOSs used. Applying the constraint on the tidal deformability of canonical neutron stars Λ1.4 = 190 +390 −120 extracted by the LIGO+VIRGO Collaborations from their improved analyses of the GW170817 event, the f-mode frequency and its damping time of canonical neutron stars are limited to 1.67 kHz -2.18 kHz and 0.155 s -0.255 s, respectively, providing a useful guidance for the ongoing search for gravitational waves from the f-mode oscillations of isolated neutron stars. Moreover, assuming either or both the f-mode frequency and its damping time will be measured precisely in future observations with advanced gravitational wave detectors, we discuss how information about the mass and/or radius as well as the still rather elusive nuclear symmetry energies at suprasaturation densities may be extracted.

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“…There are also theoretical and experimental efforts to determine the high-density EOS parameters. However, they are still very uncertain [58,63]. Nevertheless, the currently known ranges of −400 ≤ K sym ≤ 100 MeV, −200 ≤ J sym ≤ 800 MeV, and −800 ≤ J 0 ≤ 400 MeV provide at least a starting point in our efforts to narrow them down using NS observables.…”

Section: An Explicitly Isospin-dependent Parametric Eos For High-densmentioning

confidence: 99%

Extracting nuclear symmetry energies at high densities from observations of neutron stars and gravitational waves

Zhang

2019

Eur. Phys. J. A

113

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By numerically inverting the Tolman-Oppenheimer-Volkov (TOV) equation using an explicitly isospin-dependent parametric Equation of State (EOS) of dense neutron-rich nucleonic matter, a restricted EOS parameter space is established using observational constraints on the radius, maximum mass, tidal deformability and causality condition of neutron stars (NSs). The constraining band obtained for the pressure as a function of energy (baryon) density is in good agreement with that extracted recently by the LIGO+Virgo Collaborations from their improved analyses of the NS tidal deformability in GW170817. Rather robust upper and lower boundaries on nuclear symmetry energies are extracted from the observational constraints up to about twice the saturation density ρ0 of nuclear matter. More quantitatively, the symmetry energy at 2ρ0 is constrained to Esym(2ρ0) = 46.9 ± 10.1 MeV excluding many existing theoretical predictions scattered between Esym(2ρ0) = 15 and 100 MeV. Moreover, by studying variations of the causality surface where the speed of sound equals that of light at central densities of the most massive neutron stars within the restricted EOS parameter space, the absolutely maximum mass of neutron stars is found to be 2.40 M⊙ approximately independent of the EOSs used. This limiting mass is consistent with findings of several recent analyses and numerical general relativity simulations about the maximum mass of the possible super-massive remanent produced in the immediate aftermath of GW170817. deformability PACS. 2 6.60.Kp 1.0 1.2 1.4 1.6 1.8 2.0 2.2 0 200 400 600 800 1.0 1.2 1.4 1.6 1.8 2.0 2.2 1.0 1.2 1.4 1.6 1.8 2.0 2.2 2.4 J sym =600 MeV J 0 =-200 MeV K sym =-400 MeV K sym =-200 MeV K sym =0 K sym =-200 MeV J 0 =-200 MeV J sym =400 MeV J sym =600 MeV J sym =800 MeV M/M sun K sym =-200 MeV J sym =600 MeV J 0

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Eddy current effects in a high field dipole

Cited by 10 publications

References 4 publications

Towards understanding astrophysical effects of nuclear symmetry energy

Towards understanding astrophysical effects of nuclear symmetry energy

GW170817 implications on the frequency and damping time of f -mode oscillations of neutron stars

Extracting nuclear symmetry energies at high densities from observations of neutron stars and gravitational waves

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