Neutrino emissivity of the nucleon direct URCA process for rotational traditional and hyperonic neutron stars

Zhang, Naibo; Wang, Shouyu; Qi, B.; Gao, Jian-Hua; Sun, Bao Yuan

doi:10.1088/1674-1137/41/7/075101

Cited by 3 publications

(2 citation statements)

References 52 publications

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“…Meanwhile, the RMF theory has been used to study the neutron stars and obtained a lot of valuable results [23][24][25][26][27][28][29]. The start of the RMF theory is an effective Lagrangian density.…”

Section: Formalismmentioning

confidence: 99%

Possible maximum mass of dark matter existing in compact stars based on the self-interacting fermionic model

Wang

Gao

et al. 2019

Int. J. Mod. Phys. D

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By assuming that only gravitation acts between dark matter (DM) and normal matter (NM), we studied DM admixed neutron stars (DANSs) using the two-fluid TOV equations. The NM and DM of compact stars are simulated by the relativistic mean field (RMF) theory and nonself-annihilating self-interacting fermionic model, respectively. The effects of the particle mass of fermionic DM m f and the interaction strength parameter y on the properties of DANSs are investigated in detail. m f and y are considered as the free parameters due to the lack of information about the particle nature of DM so far. For a DANS, we suggest a simple universal relationship M max D = (0.267y + 0.627 − 3.21 M N M )( 1GeV m f ) 2 M for y > 100, where M max D is the maximum mass of DM existing in DANSs and M N is the mass of the neutron star without DM. For free fermion DM model (y=0), the relationship becomes M max D = (0.627 − 0.027 M 2 N M 2 )( 1GeV m f ) 2 M . The radius of DM R D shows a linear relationship with M max D in DANSs, namely R D = (7.02 M max D M + 1.36) km. These conclusions are independent of the different NM EOSs from RMF theory. Such a kind of universal relationship connecting the nature of DM particle and mass of stars might shed light on the constraining the nature of the DM by indirect method.

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Section: Formalismmentioning

confidence: 99%

Possible maximum mass of dark matter existing in compact stars based on the self-interacting fermionic model

Wang

Gao

et al. 2019

Int. J. Mod. Phys. D

Self Cite

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“…During the past decades, the covariant density functional (CDF) theory has proved to be very successful in describing the nuclear structure, nuclear excitation and decay modes . As for nuclear matter, the static as well as the rotating neutron star properties have been studied based on the CDF theory [50][51][52][53][54][55][56][57][58][59][60][61][62][63][64][65][66]. At present, the relativistic mean field (RMF) approach, as a most popular version of CDF theory, has been extended to include the isovector scalar channel in the meson-nucleon couplings, i.e., δ meson [56,[67][68][69][70].…”

Section: Introductionmentioning

confidence: 99%

Moments of inertia of neutron stars in relativistic mean field theory: The role of the isovector scalar channel

Qian

Xin

Sun

2018

Sci. China Phys. Mech. Astron.

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With the inclusion of the isovector scalar channel in the meson-nucleon couplings, taking DD-MEδ as an effective interaction, the moments of inertia of neutron stars possessing various stellar masses are studied within the density dependent relativistic mean field (RMF) theory. The isovector scalar channel contributes to the softening of the neutron-star matter equation of state (EOS) and therefore the reduction of the maximum mass and radius of neutron stars. Smaller values of the total moment of inertia I and the crustal moment of inertia ∆I are then obtained in DD-MEδ via numerical procedure in comparison with those in other selected RMF functionals. In addition, the involvement of the isovector scalar channel lowers the thickness of the neutron star crust and its mass fraction as well. The sensitivity to both the crustal mass and stellar radius causes the crustal moment of inertia to be more obviously reduced than the total one, eventually leading to a suppression on the fraction of crustal moment of inertia ∆I/I in DD-MEδ. The results indicate the crustal moment of inertia as a more sensitive probe of the neutron-star matter EOS than the total one, and demonstrate that the isovector scalar meson-nucleon couplings in the RMF theory could exert influence over the physics of pulsar glitches. neutron star, moment of inertia, relativistic mean field theory, isovector scalar channel PACS number(s): 21.60.Jz, 26.60.-c, 26.60.Kp, 26.60.Gj, 97.60.Gb, 97.10.Kc Citation: Qian Z, Xing R Y and Sun B Y, Moments of inertia of neutron stars in relativistic mean field theory: the role of the isovector scalar channel, Sci.

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Effects of free parameterized TOV equations on properties of neutron stars with hyperons

Li,

Ding,

Wei

et al. 2024

Int. J. Mod. Phys. E

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In view of the crucial role of the structure in neutron star (NS) research, parameterized TOV (PTOV) equations are used to calculate the static NS sequence with five parameters including [Formula: see text], [Formula: see text], [Formula: see text], [Formula: see text] and [Formula: see text], which represent the five factors that impact the NS structure. In order to promote the efficiency in the combination of astronomical observations and the theory, we investigate the meticulous influences of the five factors on NS structure with various hyperons in this work. Results show that the maximum masses of NSs are reduced with the free parameters, respectively, whereas the variation trend of corresponding radii is wavy in some cases. Especially, when hyperons are included, the macroscopic properties of NSs, except redshift, are relatively smaller than those in conventional NS matter. The effects on conventional NSs and hyperonic NSs are quite different in the high NS mass area but diminish when the stellar mass is lower than approximately 1.5 times solar mass. Finally, comparing with observations, we predict constraints on the free parameters.

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Neutrino emissivity of the nucleon direct URCA process for rotational traditional and hyperonic neutron stars

Abstract: Neutrino emissivity of the nucleon direct URCA process for rotational traditional and hyperonic neutron stars * Nai-Bo Zhang( ) 1 Shou-Yu Wang( ) 1;1) Bin Qi( ) 1;2) Jian-Hua Gao() 1 Bao-Yuan Sun( ) 2

Cited by 3 publications

References 52 publications

Possible maximum mass of dark matter existing in compact stars based on the self-interacting fermionic model

Possible maximum mass of dark matter existing in compact stars based on the self-interacting fermionic model

Moments of inertia of neutron stars in relativistic mean field theory: The role of the isovector scalar channel

Effects of free parameterized TOV equations on properties of neutron stars with hyperons

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