Short introduction to the physics of neutron stars

Vidaña, Isaac

doi:10.1051/epjconf/202022701018

Cited by 7 publications

(6 citation statements)

References 21 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Neutron Stars (NS) are natural laboratories to probe the behaviour of matter under extreme conditions, such as ultra-high densities, rapid rotation or ultrastrong magnetic fields [1][2][3]. With the interior composition of the NS core uncertain, it is conjectured that strangeness in the form of hyperons, meson condensates or even deconfined quark matter may appear at such high densities, which can affect several NS observable properties.…”

Section: Introductionmentioning

confidence: 99%

General relativistic treatment of $f$-mode oscillations of hyperonic stars

Pradhan,

Chatterjee,

Lanoye

et al. 2022

Preprint

View full text Add to dashboard Cite

We present a systematic study of f -mode oscillations in neutron stars containing hyperons, extending recent results obtained within the Cowling approximation to linearized General Relativity. Employing a relativistic mean field model, we find that the Cowling approximation can overestimate the quadrupolar f -mode frequency of neutron stars by up to 30% compared to the frequency obtained in the linearized general relativistic formalism. Imposing current astrophysical constraints, we derive updated empirical relations for gravitational wave asteroseismology. The frequency and damping time of quadrupole f -mode oscillations of hyperonic stars are found to be in the range of 1.47 -2.45kHz and 0.13 -0.51 sec respectively. Our correlation studies demonstrate that among the various parameters of the nucleonic and hyperonic sectors of the model, the nucleon effective mass shows the strongest correlation with mode characteristics and neutron star observables. Estimates for the detectability of f -modes in a transient burst of gravitational waves from isolated hyperonic stars is also provided.

show abstract

Section: Introductionmentioning

confidence: 99%

General relativistic treatment of $f$-mode oscillations of hyperonic stars

Pradhan,

Chatterjee,

Lanoye

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…Here, it is discovered that the relativistic mass density of the gravitational field on the surface of a neutron star is 2.65 × 10 16 ~5.87 × 10 18 𝑘𝑔𝑚 −3 which can be larger than the mass density of the neutron stars (~10 17 𝑘𝑔𝑚 −3 ). [3,4] And, the total relativistic mass of the gravitational field of the Sun or a neutron star is ~10 7 times the mass of the Sun or is ~10 21 times that of the neutron star. For different stars, the relativistic mass of the gravitational field is larger as the mass density of the star is larger.…”

Section: 𝜋𝐺mentioning

confidence: 99%

“…Table 2. The density of the stars and the relativistic mass of the fields Red giant star [11] Sun White dwarf star [12] Neutron star [3,4] ρ(10 Table 2 and Figure 3 is helpful to estimate the total relativistic mass of the gravitational fields in a galaxy.…”

Section: 𝜋𝐺mentioning

confidence: 99%

Relativistic Mass of Gravitational Field

Zhu¹

2021

Preprint

View full text Add to dashboard Cite

It is discovered that the gravitational field on the surface of a neutron star is with a relativistic mass density of 2.65*1016~5.87*1018kgm-3 which can be larger than the mass density of the neutron star (~1017kgm-3). And, the total relativistic mass of the gravitational field of the Sun is ~107 times the mass of the Sun. For different stars, the relativistic mass of the gravitational field is larger as the mass density of the star is larger. In the Milky Way, the total relativistic mass of the gravitational fields is much larger than the total mass of the stars, planets and gas. And, the relativistic mass density of the observed strongest magnetic field is 2.17*108kgm-3. This discovery should be a new frame to understand the fundamental problem of physics.

show abstract

“…Heavy-ion collision experiments in particle accelerators can reach densities up to several times 0 , but both heavy-ion and nuclear experiments probe symmetric nuclear matter (equal number of neutrons and protons) while neutrons star are highly isospin-asymmetric. This introduces uncertainties due to the extrapolation of our current knowledge of nuclear interactions to unknown territories of high densities and asymmetries [1,2] .…”

Section: Introductionmentioning

confidence: 99%

Role of vector self-interaction in Neutron Star properties

Pradhan¹,

Chatterjee²,

Gandhi³

et al. 2022

Preprint

View full text Add to dashboard Cite

Previous studies have claimed that there exist correlations among certain nuclear saturation parameters and neutron star observables, such as the slope of the symmetry energy and the radius of a 1.4 ⊙ neutron star. However, it is not clear whether such correlations are physical or spurious, as they are not observed universally for all equation of state models. In this work, we probe the role of vector self-interaction within the framework of the Relativistic Mean Field model and its role in governing the observable stellar properties and their correlations with nuclear parameters. We confirm that the effect of this term is not only to control the high density properties of the equation of state but also in governing such correlations. We also impose a limit on the maximum strength of the vector self-interaction using recent astrophysical data.

show abstract

Short introduction to the physics of neutron stars

Cited by 7 publications

References 21 publications

General relativistic treatment of $f$-mode oscillations of hyperonic stars

General relativistic treatment of $f$-mode oscillations of hyperonic stars

Relativistic Mass of Gravitational Field

Role of vector self-interaction in Neutron Star properties

Contact Info

Product

Resources

About