Is the remnant of GW190425 a strange quark star?

Sedaghat, J.; Zebarjad, S. M.; Bordbar, G. H.; Panah, B. Eslam; Moradi, R.

doi:10.1016/j.physletb.2022.137388

Cited by 8 publications

(5 citation statements)

References 64 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…5, the maximum in massive gravity goes up to the interval 2.95M ⊙ − 3.5M ⊙ , which can be located within the mass gap range, 2.5M ⊙ − 5M ⊙ . This result, in addition to covering the observational constraints, can be a candidate for the massive unseen companion in the binary system 2MASS J05215658+4359220 whose mass range is estimated to be 3.3 +2.8 −0.7 M ⊙ [62], and remnant mass of GW190425 [82,83]. To calculate compactness σ = R sch /R, one needs to obtain the Schwarzschild radius R sch in the massive gravity.…”

Section: Maximum Mass Compactness and Surface Redshiftmentioning

confidence: 93%

Effect of massive graviton on dark energy star structure

Tudeshki¹,

Bordbar²,

Panah³

2023

Preprint

View full text Add to dashboard Cite

The presence of massive gravitons in the field of massive gravity is considered as an important factor in investigating the structure of compact objects. Hence, we are encouraged to study the dark energy star structure in the Vegh's massive gravity. We consider that the equation of state governing the inner spacetime of the star is the extended Chaplygin gas, and then using this equation of state, we numerically solve the Tolman-Oppenheimer-Volkoff (TOV) equation in massive gravity. In the following, assuming different values of free parameters defined in massive gravity, we calculate the properties of dark energy star such as radial pressure, transverse pressure, anisotropy parameter, and other characteristics. Then, after obtaining the maximum mass and its corresponding radius, we compute redshift and compactness. The obtained results show that for this model of dark energy star, the maximum mass and its corresponding radius depend on the massive gravity's free parameters and anisotropy parameter. These results are consistent with the observational data, and cover the lower mass gap. We also demonstrate that all energy conditions are satisfied for this model, and in the presence of anisotropy, the dark energy star is potentially unstable.

show abstract

Section: Maximum Mass Compactness and Surface Redshiftmentioning

confidence: 93%

Effect of massive graviton on dark energy star structure

Tudeshki¹,

Bordbar²,

Panah³

2023

Preprint

View full text Add to dashboard Cite

show abstract

“…The numerical values of central density, surface density, central pressure, 𝛼, 𝛽, u(R) and z s (R) for the compact star SMC X-4 [74] for different values of 'a'. ] , (51) where,…”

Section: Nature Of Pressure and Densitymentioning

confidence: 99%

“…{3}_{-0.7}^{+2.8}{M}_{\odot}$ [ 38 ] and remnant mass of GW190425. [ 39,51 ] Carvalho et al. [ 52 ] proposed a quark star model in the non‐minimal geometry‐matter coupling (GMC) theory of gravity, and from their analysis the authors show that when

\sigma =50\hspace*{3.33333pt}k{m}^{2}

, the GMC theory can achieve the mass

2.6\hspace*{3.33333pt}{M}_{\odot}

which lies in the “mass gap” range and can describe the mass of the pulsars PSR J2215+5135, PSR J1614‐2230, PSR J0952‐0607 and of the secondary object in the GW190814 event.…”

Section: Introductionmentioning

confidence: 99%

“…In very recent work, Tudeshki et al [37] discussed the effect of massive graviton on dark energy star structure, and by analyzing M − R curve, they show that the maximum mass in massive gravity goes up to the interval (2.95 − 3.5)M ⊙ , which can be located within the mass gap range, (2.5 − 5)M ⊙ and this result, covers the observational constraints and can be a candidate for the massive unseen companion in the binary system 2MASS J05215658+4359220 whose mass range is estimated to be 3.3 +2.8 −0.7 M ⊙ [38] and remnant mass of GW190425. [39,51] Carvalho et al [52] proposed a quark star model in the non-minimal geometry-matter coupling (GMC) theory of gravity, and from their analysis the authors show that when 𝜎 = 50 km 2 , the GMC theory can achieve the mass 2.6 M ⊙ which lies in the "mass gap" range and can describe the mass of the pulsars PSR J2215+5135, PSR J1614-2230, PSR J0952-0607 and of the secondary object in the GW190814 event. From the analysis of Pretel, [42] the mass of the dark energy star lies in the "mass gap" range that can be achieved by using a Chaplygin-like equation of state in the General theory of relativity.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Existence of Dark Energy Stars within Lower Mass Gap in the Realm of f(Q)$f(Q)$ Gravity

Bhar

2023

Fortschritte der Physik

View full text Add to dashboard Cite

The object of this article is to study a new class of dark energy stars in the background of gravity by using the metric potentials proposed by Krori‐Barua [J. Phys. A, Math. Gen. 8:508 (1975)]. To achieve the goal, a quadratic form of as is taken into account for the static spherically symmetric spacetime,`a' being a coupling parameter of gravity. The maximum allowable masses with corresponding radii have been obtained via plots for and 8. The obtained maximum masses from our analysis are found in the range . For a smaller value of the coupling parameter ‘a’ associated with gravity, more massive stars are found. The radii corresponding to the maximum masses also increase with decreasing ‘a’. In particular, when , the theory can achieve a dark energy star of mass for certain specific combinations of model parameters. This obtained mass is located within a mass in the range of and that can be a lighter object in the GW190814 event detected by LIGO/VIRGO experiments.

show abstract

“…As the details of the nuclear models are out of the scope of this work, we refer to Refs. [28][29][30][31][32][33][34][35] and references within for more information.…”

Section: Introductionmentioning

confidence: 99%

Bayesian Exploration of Phenomenological EoS of Neutron/Hybrid Stars with Recent Observations

et al. 2023

View full text Add to dashboard Cite

The description of the stellar interior of compact stars remains as a big challenge for the nuclear astrophysics community. The consolidated knowledge is restricted to density regions around the saturation of hadronic matter ρ0=2.8×1014gcm−3, regimes where our nuclear models are successfully applied. As one moves towards higher densities and extreme conditions up to the quark/gluons deconfinement, little can be said about the microphysics of the equation of state (EoS). Here, we employ a Markov Chain Monte Carlo (MCMC) strategy to access the variability at high density regions of polytropic piecewise models for neutron star (NS) EoS or possible hybrid stars, i.e., a NS with a small quark-matter core. With a fixed description of the hadronic matter for low density, below the nuclear saturation density, we explore a variety of models for the high density regimes leading to stellar masses near to 2.5M⊙, in accordance with the observations of massive pulsars. The models are constrained, including the observation of the merger of neutrons stars from VIRGO-LIGO and with the pulsar observed by NICER. In addition, we also discuss the possibility of the use of a Bayesian power regression model with heteroscedastic error. The set of EoS from the Laser Interferometer Gravitational-Wave Observatory (LIGO) was used as input and treated as the data set for the testing case.

show abstract

Is the remnant of GW190425 a strange quark star?

Cited by 8 publications

References 64 publications

Effect of massive graviton on dark energy star structure

Effect of massive graviton on dark energy star structure

Existence of Dark Energy Stars within Lower Mass Gap in the Realm of f(Q)$f(Q)$ Gravity

Bayesian Exploration of Phenomenological EoS of Neutron/Hybrid Stars with Recent Observations

Contact Info

Product

Resources

About