Exact solutions of a model for strange stars with interacting quarks

Rocha, L. S.; Bernardo, A.; Avellar, Marcio G. B. de; Horvath, J. E.

doi:10.1002/asna.201913584

Cited by 18 publications

(9 citation statements)

References 11 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…8. Similar plots and comparisons have been found in the literature for linearly approximated EoS's [23] and the more recently pursued CFL EoS [24][25][26]. It is interesting to note that the quadratic EoS mimics the CFL EoS more closely than the linear EoS.…”

Section: Discussionsupporting

confidence: 81%

Stability and improved physical characteristics of relativistic compact objects arising from the quadratic term in $$p_r = \alpha \rho ^2 + \beta \rho - \gamma $$

Thirukkanesh¹,

Bogadi

Govender

et al. 2021

Eur. Phys. J. C

View full text Add to dashboard Cite

We investigate the stability and enhancement of the physical characteristics of compact, relativistic objects which follow a quadratic equation of state. To achieve this, we make use of the Vaidya–Tikekar metric potential. This gravitational potential has been shown to be suitable for describing superdense stellar objects. Pressure anisotropy is also a key feature of our model and is shown to play an important role in maintaining stability. Our results show that the combination of the Vaidya–Tikekar gravitational potential used together with the quadratic equation of state provide models which are favourable. In comparison with other equations of state, we have shown that the quadratic equation of state mimics the colour-flavour-locked equation of state more closely than the linear equation of state.

show abstract

Section: Discussionsupporting

confidence: 81%

Stability and improved physical characteristics of relativistic compact objects arising from the quadratic term in $$p_r = \alpha \rho ^2 + \beta \rho - \gamma $$

Thirukkanesh¹,

Bogadi

Govender

et al. 2021

Eur. Phys. J. C

View full text Add to dashboard Cite

show abstract

“…By appealing to the microphysics associated with strange matter, Rocha et al [184] and many others adopted a CFL EoS of the form…”

Section: Colour-flavour-locked Equation Of Statesmentioning

confidence: 99%

“…Working Rule : Rocha et al [184,185]: The authors have provided two anisotropic models made of CFL strange matter. The strange matter is assumed to be composed of strange quarks in addition to the usual ups and downs, having an energy per baryon lower than the strangeness counterpart, and even lower than that of nuclear matter.…”

Section: Colour-flavour-locked Equation Of Statesmentioning

confidence: 99%

The classification of interior solutions of anisotropic fluid configurations

Kumar¹,

Bharti²

2021

Preprint

View full text Add to dashboard Cite

The solutions of the Einstein-Maxwell system of equations, useful for the modeling of compact stars have a long and rich history. It took just a year since Einstein's general theory of relativity was published for Karl Schwarzschild to obtain the first exact solution of Einstein's field equations. The number of viable exact solutions has been growing since then. Different models have been constructed for a variety of applications. In this article, we have discussed different ways of generating a static spherically symmetric anisotropic fluid model. The purpose of the present article is to present a simple classification scheme for static and spherically symmetric anisotropic fluid solutions. The known solutions are reviewed and compartmentalized according to this scheme so that we can illustrate general ideas about these solutions without being exhaustive.

show abstract

“…When n = 1/2 and η = 0, then we regain a color-flavorlocked (CFL) equation of state of Rocha et al (2019) p r = α…”

Section: The Modelmentioning

confidence: 99%

“…Since Wittten's work on quark matter (Witten (1984)) many investigations have been conducted in order to describe realistic physical features of these stellar compact objects. For more details see Haensel et al (1986), Alcock et al (1986), Benvenuto and Horvath (1989), Horvath (2002, 2003), Alford et al (2005), Bodmer (1971), Terazawa et al (1978) and Rocha et al (2019). The discovery of new observed pulsars with mass above 1.97 M challenges the theoretical approach in describing compact stars.…”

mentioning

confidence: 99%

Model of compact star with ordinary and dark matter

Takisa

Leeuw

Maharaj

2020

Astrophys Space Sci

View full text Add to dashboard Cite

We study compact stars formed by dark and ordinary matter, with attributes of both neutron star matter and quark star matter. We assume an equation of state for dark matter which is consistent with the rotational curves of galaxies and for color-flavor-locked (CFL) distributions for ordinary matter. This is done in the curved Krori-Barua spacetime geometry in general relativity. We find new exact solutions of dark matter admixed compact objects, with maximum mass 2.67 M and radius around 11.16 km, with 52.40% of dark matter content. By varying the dark matter ratio, we obtain the masses of dark compact stars with masses less than 2.67 M . Keywords Einstein equations • Compact stars • Equation of state 1 IntroductionA quark star is made up of self-bound strange quark matter and its also known as a hypothetical stellar object (see

show abstract

Exact solutions of a model for strange stars with interacting quarks

Cited by 18 publications

References 11 publications

Stability and improved physical characteristics of relativistic compact objects arising from the quadratic term in $$p_r = \alpha \rho ^2 + \beta \rho - \gamma $$

Stability and improved physical characteristics of relativistic compact objects arising from the quadratic term in $$p_r = \alpha \rho ^2 + \beta \rho - \gamma $$

The classification of interior solutions of anisotropic fluid configurations

Model of compact star with ordinary and dark matter

Contact Info

Product

Resources

About