scholarly journals The I-Love-Q Relations for Superfluid Neutron Stars

Universe ◽  
2021 ◽  
Vol 7 (4) ◽  
pp. 111
Author(s):  
Cheung-Hei Yeung ◽  
Lap-Ming Lin ◽  
Nils Andersson ◽  
Greg Comer
Keyword(s):  
Fluid Dynamics ◽  
Equation Of State ◽  
Neutron Stars ◽  
Quadrupole Moment ◽  
Fluid Model ◽  
Normal Component ◽  
Approximate Equation ◽  
Mean Field Model ◽  
Polytropic Model ◽  
Two Fluid

The I-Love-Q relations are approximate equation-of-state independent relations that connect the moment of inertia, the spin-induced quadrupole moment, and the tidal deformability of neutron stars. In this paper, we study the I-Love-Q relations for superfluid neutron stars for a general relativistic two-fluid model: one fluid being the neutron superfluid and the other a conglomerate of all charged components. We study to what extent the two-fluid dynamics might affect the robustness of the I-Love-Q relations by using a simple two-component polytropic model and a relativistic mean field model with entrainment for the equation-of-state. Our results depend crucially on the spin ratio Ωn/Ωp between the angular velocities of the neutron superfluid and the normal component. We find that the I-Love-Q relations can still be satisfied to high accuracy for superfluid neutron stars as long as the two fluids are nearly co-rotating Ωn/Ωp≈1. However, the deviations from the I-Love-Q relations increase as the spin ratio deviates from unity. In particular, the deviation of the Q-Love relation can be as large as O(10%) if Ωn/Ωp differ from unity by a few tens of percent. As Ωn/Ωp≈1 is expected for realistic neutron stars, our results suggest that the two-fluid dynamics should not affect the accuracy of any gravitational waveform models for neutron star binaries that employ the relation to connect the spin-induced quadrupole moment and the tidal deformability.

Thermodynamic excess functions of regular and related solutions according to some equations of state based on the perturbed hard sphere model

1973 ◽  
Vol 26 (10) ◽  
pp. 2071 ◽  
Author(s):  
DK Astin ◽  
ID Watson
Keyword(s):  
Equation Of State ◽  
Hard Sphere ◽  
Equations Of State ◽  
Fluid Model ◽  
Quantitative Agreement ◽  
Excess Functions ◽  
Hard Sphere Model ◽  
Thermodynamic Excess Functions ◽  
Two Fluid Model ◽  
Two Fluid

The excess thermodynamic functions of 12 mixtures, each representative of a certain type of system, have been calculated by means of the van der Waals, Frisch,1 and Carnahan and Starling2 equation of state, in conjunction with one-fluid and two-fluid models of conformal mixtures. In addition, the equation of state of hard sphere mixtures of Mansoori et al.3 has been used. Though none of the approaches give quantitative agreement for any of the systems considered, they all give a qualitative account which broadly reflect the trends in behaviour. In the cases where it is appropriate to comment on the qualitative accuracy the two-fluid model, used with either the Frisch or Carnahan and Starling equation of state, shows a slight superiority to the others.

scholarly journals Double dark matter admixed neutron star

2018 ◽  
Vol 27 (16) ◽  
pp. 1950002 ◽  
Author(s):  
Zeinab Rezaei
Keyword(s):  
Dark Matter ◽  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Equations Of State ◽  
Compact Object ◽  
Gravitational Redshift ◽  
Two Fluid

The dark matter (DM) in neutron stars can exist from the lifetime of the progenitor or when captured by this compact object. The properties of DM that enter the neutron stars through each step could be different from each other. Here, we investigate the structure of neutron stars which are influenced by the DM in two processes. Applying a generalization of two-fluid formalism to three-fluid one and the equation-of-state from the rotational curves of galaxies, we explore the structure of double DM admixed neutron stars. The behavior of the neutron and DM portions for these stars is considered. In addition, the influence of the DM equations of state on the stars with different contributions of visible and DM are studied. The gravitational redshift of these stars in different cases of DM equations of state is investigated.

On Treatment of Negative Pressures in Fluid Dynamics

2005 ◽  
Author(s):  
Iztok Tiselj ◽  
Janez Gale
Keyword(s):  
Fluid Dynamics ◽  
Phase Transition ◽  
Two Phase Flow ◽  
Fluid Model ◽  
Saturation Pressure ◽  
Phase Flow ◽  
Two Phase ◽  
Negative Pressures ◽  
Two Fluid Model ◽  
Two Fluid

Rapid depressurization of a cold single-phase liquid leads to the onset of a vaporisation, i.e. the phase transition phenomena. Prior to the start and in the very first moment of the phase transition, pressure in the liquid may briefly drop to negative values, when initial liquid temperature is low enough. Metastable liquid in a state of tension is well known in static experiments, but is less known in the fluid dynamics. The present paper discusses some preliminary findings in the field of modeling of the negative pressures in transient water flows and subsequent phase transition with a single-pressure two-fluid model. A highly simplified single-pressure two-fluid model is used in the present work to describe the two-phase flow with negative liquid and positive vapor pressure. The assumption used at negative liquid pressures is equal temperature of liquid and newly generated vapor phase, while the gas pressure is assumed to be the saturation pressure at that temperature. Rather rough models seem to be sufficiently accurate due to the large uncertainty in the modeling of the single-to-two-phase flow transition, which strongly depends on the density of the nucleation sites in the liquid and at the wall.

Simplified two-group two-fluid model for three-dimensional two-phase flow Computational Fluid Dynamics for vertical upward flow

2018 ◽  
Vol 108 ◽  
pp. 503-516 ◽  
Author(s):  
Takashi Hibiki ◽  
Joshua P. Schlegel ◽  
Tetsuhiro Ozaki ◽  
Shuichiro Miwa ◽  
Somboon Rassame
Keyword(s):  
Fluid Dynamics ◽  
Computational Fluid Dynamics ◽  
Two Phase Flow ◽  
Fluid Model ◽  
Three Dimensional ◽  
Phase Flow ◽  
Upward Flow ◽  
Two Phase ◽  
Two Fluid Model ◽  
Two Fluid

scholarly journals Anisotropic neutron stars with hyperons: implication of the recent nuclear matter data and observations of neutron stars

2020 ◽  
Vol 80 (8) ◽  
Author(s):  
A. Rahmansyah ◽  
A. Sulaksono ◽  
A. B. Wahidin ◽  
A. M. Setiawan
Keyword(s):  
Equation Of State ◽  
Neutron Stars ◽  
Mean Field ◽  
Coupling Constants ◽  
Anisotropic Pressure ◽  
Recent Experimental Data ◽  
Observation Data ◽  
Anisotropic Model ◽  
Mean Field Model ◽  
Anisotropic Models

Abstract Motivated by a recent report by Biwas and Bose (Phys Rev D 99:104002, 2019) that the observations of GW170817 to constrain the extent of pressure anisotropy in neutron stars within Bower–Liang anisotropic model, we systematically study the effects of anisotropic pressure on properties of the neutron stars with hyperons. The equation of state is calculated using the relativistic mean-field model with a BSP parameter set to determine nucleonic coupling constants and by using SU(6) and hyperon potential depths to determine hyperonic coupling constants. We investigate three models of anisotropic pressure known in literature namely Bowers and Liang (Astrophys J 88:657, 1974), Horvat et al. (Class Quant Grav 28:025009, 2011), and Cosenza et al. (J Math Phys (NY) 22:118, 1981). The reliability of the equation of state used is checked by comparing the parameters of the corresponding EOS to recent experimental data. The mass–radius, moment of inertia, and tidal deformability results of Bowers–Liang, Horvat et al., and Cosenza et al. anisotropic models are compared to the corresponding recent results extracted from the analysis of some NS observation data. We have found that the radii predicted by anisotropic NS are sensitive to the anisotropic model used and the results obtained by using the model proposed by Horvat et al. with anisotropic free parameter $$\varUpsilon ~\approx -$$Υ≈- 1.15 are relative compatible with all taken constraints.

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