High-Density Matter in the Chiral Sigma Model

Sahu, P. K.; Basu, Rahul; Datta, Bithin

doi:10.1086/173233

Cited by 60 publications

(90 citation statements)

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“…The A18+δv+UIX model additionally includes three-nucleon interactions described by the Urbana IX [UIX] model (Pudliner et al , 1995) and the effect of relativistic boost corrections. The second nucleonic EoS model (N2; Sahu et al (1993); Table 2), which is harder ( § 1) than N1, is a field theoretical EoS for nucleonic matter in β-equilibrium based on the chiral sigma model. The model includes an isoscalar vector field generated dynamically.…”

Section: Pulsars and Equations Of Statementioning

confidence: 99%

Millisecond radio pulsars with known masses: Parameter values and equation of state models

et al. 2017

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The recent fast growth of a population of millisecond pulsars with precisely measured mass provides an excellent opportunity to characterize these compact stars at an unprecedented level. This is because the stellar parameter values can be accurately computed for known mass and spin rate and an assumed equation of state (EoS) model. For each of the 16 such pulsars and for a set of EoS models from nucleonic, hyperonic, strange quark matter and hybrid classes, we numerically compute fast spinning stable stellar parameter values considering the full effect of general relativity. This first detailed catalogue of the computed parameter values of observed millisecond pulsars provides a testbed to probe the physics of compact stars, including their formation, evolution and EoS. We estimate uncertainties on these computed values from the uncertainty of the measured mass, which could be useful to quantitatively constrain EoS models. We note that the largest value of the central density ρ c in our catalogue is ∼ 5.8 times the nuclear saturation density ρ sat , which is much less than the expected maximum value 13ρ sat . We argue that the ρ c -values of at most a small fraction of compact stars could be much larger than 5.8ρ sat . Besides, we find that the constraints on EoS models from accurate radius measurements could be significantly biased for some of our pulsars, if stellar spinning configurations are not used to compute the theoretical radius values.

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Section: Pulsars and Equations Of Statementioning

confidence: 99%

Millisecond radio pulsars with known masses: Parameter values and equation of state models

et al. 2017

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“…However, a dynamical mass generation mechanism of the ρ−meson in a similar manner will not generate the correct symmetry energy. Therefore, we have taken an explicit mass term for the isovector ρ−meson similar to what was considered in earlier works [20,21,22,23].…”

Section: The Equation Of Statementioning

confidence: 99%

Attributes of a rotating neutron star with a hyperon core

2008

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We study the effect of rotation on global properties of neutron star with a hyperon core in an effective chiral model with varying nucleon effective mass within a mean field approach. The resulting gross properties of the rotating compact star sequences are then compared and analyzed with other theoretical predictions and observations from neutron stars. The maximum mass of the compact star predicted by the model lies in the range (1.4 − 2.4) M⊙ at Kepler frequency ΩK , which is consistent with recent observation of high mass stars thereby reflecting the sensitivity of the underlying nucleon effective mass in the dense matter EoS. We also discuss the implications of the experimental constraints from the flow data from heavy-ion collisions on the global properties of the rotating neutron stars.

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“…The beauty of this model is that its non-linear terms simulate the three body forces and is essential to reproduce the nuclear matter saturation properties. A decade ago we proposed a SU(2) CS model, where the mass of the isoscalar vector field is generated dynamically [19]. The main problem of this theory was unrealistic high incompressibility.…”

Section: Introductionmentioning

confidence: 99%

Hot nuclear matter in asymmetry chiral sigma model

et al. 2004

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In the frame work of SU(2) chiral sigma model, the nuclear matter properties at zero and finite temperature have been investigated. We have analyzed the nuclear matter equation of state by varying different parameters, which agrees well with the one derived from the heavy-ion collision experiment at extreme densities and reliable realistic(DBHF) model at low density region. We have then calculated the temperature dependent asymmetric nuclear matter, also investigated the critical temperature of liquid gas phase transition and compared with the experimental data. We found that the critical temperature in our model is in the range of 14−20 MeV.

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High-Density Matter in the Chiral Sigma Model

Cited by 60 publications

References 0 publications

Millisecond radio pulsars with known masses: Parameter values and equation of state models

Millisecond radio pulsars with known masses: Parameter values and equation of state models

Attributes of a rotating neutron star with a hyperon core

Hot nuclear matter in asymmetry chiral sigma model

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