In this work,we have explored wormhole(WH)solutions in F(R,L_(m))gravity by assuming the Morris-Thorne WH metric and F(R,Lm)=R/2+(1+γR)L_(m),whereγis the free model parameter.We determined the WH solutions by utiliz...In this work,we have explored wormhole(WH)solutions in F(R,L_(m))gravity by assuming the Morris-Thorne WH metric and F(R,Lm)=R/2+(1+γR)L_(m),whereγis the free model parameter.We determined the WH solutions by utilizing two newly developed shape functions(SF)that satisfy all basic conditions for a WH’s physical validity.We also observe that the null energy condition(NEC)behaves negatively.Finally,for both models,we use the volume integral quantifier(VIQ)and Tolman-Oppenheimer-Volkoff(TOV)equation to determine how much exotic matter is needed near the WH throat and the stability of the WH.The extensive detailed discussions of the matter components have been done via graphical analysis.The obtained WH geometries meet the physically acceptable conditions for a stable wormhole.展开更多
In the background of f(R,L_(m))gravity,this work investigates three distinct dark matter halo profiles to test the possibility of generalised wormhole geometry within the galactic halo regions.The current study aims t...In the background of f(R,L_(m))gravity,this work investigates three distinct dark matter halo profiles to test the possibility of generalised wormhole geometry within the galactic halo regions.The current study aims to accomplish these goals by examining various dark matter profiles including universal rotation curves(URC),Navarro-Frenk-White(NFW)model-Ⅰ,and NFW model-Ⅱinside two distinct f(R,L_(m))gravity models.According to the f(R,L_(m))=R/2+L^(a)_(m)model,the dark matter(DM)halo density profiles produce suitable shape functions that meet all the necessary requirements for exhibiting the wormhole geometries with appropriate choice of free parameters.In addition,to examine DM profiles under the f(R,L_(m))=R/2+(1+λR)L_(m) model,we consider a specific shape function.Further,we observed that the derived solution from both two models violates the null energy constraints,confirming that the DM supports wormholes to maintain in the galactic halo.展开更多
This study uses a minimal geometric deformation scheme within the f(R,L_(m),T)gravity paradigm to model anisotropic compact stars using class-1 embedding spacetime.We introduce the deformation of the radial component ...This study uses a minimal geometric deformation scheme within the f(R,L_(m),T)gravity paradigm to model anisotropic compact stars using class-1 embedding spacetime.We introduce the deformation of the radial component of the metric tensor,which decouples the Einstein field equations and introduces an additional gravitational source.The relevant constants are evaluated using observational data from seven realistic star candidates by matching the inner region with the outer Schwarzschild line element.A comprehensive graphical analysis of three compact stars is performed to examine the impact of the coupling parameter β and deformation parameter n,revealing positive,well-behaved energy densities and pressures that satisfy the energy conditions.The study found that negative values of the coupling parameter β allow greater mass accumulation while preserving key physical characteristics,such as stability under Herrera's cracking condition and the extended Tolman-Oppenheimer-Volkoff equation.This study highlights the significance of gravitational decoupling for determining mass,redshift,and compactness and provides important insights into the internal structure of stellar bodies within this new generalized gravity framework.展开更多
We investigate the physical properties of quark stars within the framework of f(R,L_(m),T)gravity.The quark matter inside these stars is modeled as de-confined quarks and described by a color-flavor-locked equation of...We investigate the physical properties of quark stars within the framework of f(R,L_(m),T)gravity.The quark matter inside these stars is modeled as de-confined quarks and described by a color-flavor-locked equation of state.Using this equation of state,we numerically solve the modified Tolman-Oppenheimer-Volkoff(TOV)equation to obtain the mass and radius of quark stars.We analyze key properties of the quark star such as dynamical stability,compactness,and gravitational redshift.The results show that the modified gravitational theory has a significant impact on the properties of quark stars and is consistent with the observational data of massive pulsars.展开更多
We investigated the impact of f(R,L_(m),T)gravity on the internal structure of compact stars,expecting this theory to manifest prominently in the high-density cores of such stars.We considered the algebraic function,f...We investigated the impact of f(R,L_(m),T)gravity on the internal structure of compact stars,expecting this theory to manifest prominently in the high-density cores of such stars.We considered the algebraic function,f(R,L_(m),T)=R+αTL_(m),whereαrepresents the matter-geometry coupling constant.We specifically chose the matter Lagrangian density L_(m)=-ρto explore compact stars with anisotropic pressure.To this end,we employed the MIT bag model as an equation of state.Subsequently,we numerically solved the hydrostatic equilibrium equations to obtain mass-radius relations for quark stars(QSs),examining static stability criteria,adiabatic index,and speed of sound.Finally,we used recent astrophysical data to constrain the coupling parameterα,which may lead to either larger or smaller masses for QSs,compared to their counterparts in general relativity.展开更多
基金S Chaudhary expresses his gratitude to the Central University of Haryana for providing a University Research Fellowship (URF) under the Reg. No. 222019the Department of Mathematics, Central University of Haryanathe University Grant Commission (UGC), New Delhi, India under the NTA Ref. No. 211610000030 for providing financial support
文摘In this work,we have explored wormhole(WH)solutions in F(R,L_(m))gravity by assuming the Morris-Thorne WH metric and F(R,Lm)=R/2+(1+γR)L_(m),whereγis the free model parameter.We determined the WH solutions by utilizing two newly developed shape functions(SF)that satisfy all basic conditions for a WH’s physical validity.We also observe that the null energy condition(NEC)behaves negatively.Finally,for both models,we use the volume integral quantifier(VIQ)and Tolman-Oppenheimer-Volkoff(TOV)equation to determine how much exotic matter is needed near the WH throat and the stability of the WH.The extensive detailed discussions of the matter components have been done via graphical analysis.The obtained WH geometries meet the physically acceptable conditions for a stable wormhole.
基金University Grant Commission(UGC),Govt.of India,New Delhi,for awarding JRF(NTA Ref.No.:191620024300)University Grants Commission(UGC),New Delhi,India,for awarding National Fellowship for Scheduled Caste Students(UGC-Ref.No.:201610123801)+1 种基金PKS acknowledges the National Board for Higher Mathematics(NBHM)under the Department of Atomic Energy(DAE),Govt.of India,for financial support to carry out the Research project No.:02011/3/2022 NBHM(R.P.)/R&D II/2152 Dt.14.02.2022IUCAA,Pune,India for providing support through the visiting Associateship program.
文摘In the background of f(R,L_(m))gravity,this work investigates three distinct dark matter halo profiles to test the possibility of generalised wormhole geometry within the galactic halo regions.The current study aims to accomplish these goals by examining various dark matter profiles including universal rotation curves(URC),Navarro-Frenk-White(NFW)model-Ⅰ,and NFW model-Ⅱinside two distinct f(R,L_(m))gravity models.According to the f(R,L_(m))=R/2+L^(a)_(m)model,the dark matter(DM)halo density profiles produce suitable shape functions that meet all the necessary requirements for exhibiting the wormhole geometries with appropriate choice of free parameters.In addition,to examine DM profiles under the f(R,L_(m))=R/2+(1+λR)L_(m) model,we consider a specific shape function.Further,we observed that the derived solution from both two models violates the null energy constraints,confirming that the DM supports wormholes to maintain in the galactic halo.
文摘This study uses a minimal geometric deformation scheme within the f(R,L_(m),T)gravity paradigm to model anisotropic compact stars using class-1 embedding spacetime.We introduce the deformation of the radial component of the metric tensor,which decouples the Einstein field equations and introduces an additional gravitational source.The relevant constants are evaluated using observational data from seven realistic star candidates by matching the inner region with the outer Schwarzschild line element.A comprehensive graphical analysis of three compact stars is performed to examine the impact of the coupling parameter β and deformation parameter n,revealing positive,well-behaved energy densities and pressures that satisfy the energy conditions.The study found that negative values of the coupling parameter β allow greater mass accumulation while preserving key physical characteristics,such as stability under Herrera's cracking condition and the extended Tolman-Oppenheimer-Volkoff equation.This study highlights the significance of gravitational decoupling for determining mass,redshift,and compactness and provides important insights into the internal structure of stellar bodies within this new generalized gravity framework.
基金Supported by the National Natural Science Foundation of China(12475057,12303079)。
文摘We investigate the physical properties of quark stars within the framework of f(R,L_(m),T)gravity.The quark matter inside these stars is modeled as de-confined quarks and described by a color-flavor-locked equation of state.Using this equation of state,we numerically solve the modified Tolman-Oppenheimer-Volkoff(TOV)equation to obtain the mass and radius of quark stars.We analyze key properties of the quark star such as dynamical stability,compactness,and gravitational redshift.The results show that the modified gravitational theory has a significant impact on the properties of quark stars and is consistent with the observational data of massive pulsars.
基金Supported by Walailak University under the New Researcher Development scheme(WU67268)A.Pradhan expresses gratitude to the IUCCA in Pune,India,for offering facilities under associateship programs.In addition,İzzet Sakallıthanks TÜBİTAK,ANKOS,and SCOAP3 for their contributions.Takol Tangphati andİzzet Sakallıalso appreciate COST Actions CA21106 and CA22113 for their networking support。
文摘We investigated the impact of f(R,L_(m),T)gravity on the internal structure of compact stars,expecting this theory to manifest prominently in the high-density cores of such stars.We considered the algebraic function,f(R,L_(m),T)=R+αTL_(m),whereαrepresents the matter-geometry coupling constant.We specifically chose the matter Lagrangian density L_(m)=-ρto explore compact stars with anisotropic pressure.To this end,we employed the MIT bag model as an equation of state.Subsequently,we numerically solved the hydrostatic equilibrium equations to obtain mass-radius relations for quark stars(QSs),examining static stability criteria,adiabatic index,and speed of sound.Finally,we used recent astrophysical data to constrain the coupling parameterα,which may lead to either larger or smaller masses for QSs,compared to their counterparts in general relativity.
