Strange quark matter fragmentation in astrophysical events

Paulucci, L.; Horvath, J. E.

doi:10.1016/j.physletb.2014.04.036

Cited by 57 publications

(44 citation statements)

References 41 publications

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“…It is observed that ignoring critical aspects of the quantum particle physics in the framework of GR several authors [91][92][93][94][95][96][97][98] successfully have been introduced this simplified form of the MIT Bag EOS to study stellar systems made of SQM.…”

Section: Basic Stellar Equations In F (R T ) Theory Of Gravitymentioning

confidence: 99%

Anisotropic strange stars under simplest minimal matter-geometry coupling in the f ( R,T ) gravity

et al. 2018

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We study strange stars in the framework of f (R, T ) theory of gravity. To provide exact solutions of the field equations it is considered that the gravitational Lagrangian can be expressed as the linear function of the Ricci scalar R and the trace of the stress-energy tensor T , i.e. f (R, T ) = R + 2χT , where χ is a constant. We also consider that the strange quark matter (SQM) distribution inside the stellar system is governed by the phenomenological MIT Bag model equation of state (EOS), given as pr = 1 3 (ρ − 4 B), where B is the Bag constant. Further, for a specific value of B and observed values of mass of the strange star candidates we obtain the exact solution of the modified Tolman-Oppenheimer-Volkoff (TOV) equation in the framework of f (R, T ) gravity and have studied in detail the dependence of the different physical parameters, like the metric potentials, energy density, radial and tangential pressures and anisotropy etc., due to the chosen different values of χ. Likewise in GR, as have been shown in our previous work [Deb et al., Ann. Phys. (Amsterdam) 387, 239 (2017)] in the present work also we find maximum anisotropy at the surface which seems an inherent property of the strange stars in modified f (R, T ) theory of gravity. To check the physical acceptability and stability of the stellar system based on the obtained solutions we have performed different physical tests, viz., the energy conditions, Herrera cracking concept, adiabatic index etc. In this work, we also have explained the effects, those are arising due to the interaction between the matter and the curvature terms in f (R, T ) gravity, on the anisotropic compact stellar system. It is interesting to note that as the values of χ increase the strange stars become more massive and their radius increase gradually so that eventually they gradually turn into less dense compact objects. The present study reveals that the modified f (R, T ) gravity is a suitable theory to explain massive stellar systems like recent magnetars, massive pulsars and super-Chandrasekhar stars, which can not be explained in the framework of GR. However, for χ = 0 the standard results of Einsteinian gravity are retrieved.

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Section: Basic Stellar Equations In F (R T ) Theory Of Gravitymentioning

confidence: 99%

Anisotropic strange stars under simplest minimal matter-geometry coupling in the f ( R,T ) gravity

et al. 2018

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“…It is observed that to describe a stellar model made of strange quark matter well known MIT bag EOS can be considered under such a situation. Successful use of the MIT bag EOS to describe strange quark stars the following recent works are available in the literature [31,32,33,34,35,36,37,38]. This type of simplest form of EOS is very useful to study equilibrium configuration of a compact stellar object made of only up, down and strange quarks even in the framework of general relativity without invoking any quantum mechanical particle physics aspect.…”

Section: Introductionmentioning

confidence: 99%

Relativistic model for anisotropic strange stars

et al. 2017

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In this article, we attempt to find a singularity free solution of Einstein's field equations for compact stellar objects, precisely strange (quark) stars, considering Schwarzschild metric as the exterior spacetime. To this end, we consider that the stellar object is spherically symmetric, static and anisotropic in nature and follows the density profile given by Mak and Harko (2002), which satisfies all the physical conditions. To investigate different properties of the ultra-dense strange stars we have employed the MIT bag model for the quark matter. Our investigation displays an interesting feature that the anisotropy of compact stars increases with the radial coordinate and attains Preprint submitted to Annals of Physics October 19, 2017 its maximum value at the surface which seems an inherent property for the singularity free anisotropic compact stellar objects. In this connection we also perform several tests for physical features of the proposed model and show that these are reasonably acceptable within certain range. Further, we find that the model is consistent with the energy conditions and the compact stellar structure is stable with the validity of the TOV equation and Herrera cracking concept. For the masses bellow the maximum mass point in mass vs radius curve the typical behavior achieved within the framework of general relativity. We have calculated the maximum mass and radius of the strange stars for the three finite values of bag constant B g .

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“…At a microscopic level, a dynamical study of the droplet boundary once formed has not been studied in detail yet. If the full NS converts to a more compact QM star this exotic type of matter would be ejected leaving an imprint on the cosmic rays or scintillation patterns [55][56][57]. Boundary conditions for isolated clusters have been somewhat explored in [58] where, arising from the strange quark content, the name of strangelet is coined.…”

Section: Resultsmentioning

confidence: 99%

Dark matter and bubble nucleation in old neutron stars

et al. 2019

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We study the probability for nucleation of quark matter droplets in the dense cold cores of old neutron stars induced by the presence of a self-annihilating dark matter component, χ. Using a parameterized form of the equation of state for hadronic and quark phases of ordinary matter, we explore the thermodynamical conditions under which droplet formation is facilitated by energy injection from χ self-annihilations. We obtain the droplet nucleation time as a function of the dark matter candidate mass, mχ. We discuss further observational consequences.I.

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Strange quark matter fragmentation in astrophysical events

Cited by 57 publications

References 41 publications

Anisotropic strange stars under simplest minimal matter-geometry coupling in the f ( R,T ) gravity

Anisotropic strange stars under simplest minimal matter-geometry coupling in the f ( R,T ) gravity

Relativistic model for anisotropic strange stars

Dark matter and bubble nucleation in old neutron stars

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