We identify an S-shaped main-jet axis in the Vela core-collapse supernova remnant(CCSNR)that we attribute to a pair of precessing jets,one of the tens of pairs of jets that exploded the progenitor of Vela according to...We identify an S-shaped main-jet axis in the Vela core-collapse supernova remnant(CCSNR)that we attribute to a pair of precessing jets,one of the tens of pairs of jets that exploded the progenitor of Vela according to the jittering jets explosion mechanism(JJEM).A main-jet axis is a symmetry axis across the CCSNR and through the center.We identify the S-shaped main-jet axis by the high abundance of ejecta elements,oxygen,neon,and magnesium.We bring the number of identified pairs of clumps and ears in Vela to seven,two pairs shaped by the pair of precessing jets that formed the main-jet axis.The pairs and the main-jet axis form the point-symmetric wind-rose structure of Vela.The other five pairs of clumps/ears do not have signatures near the center,only on two opposite sides of the CCSNR.We discuss different possible jet-less shaping mechanisms to form such a point-symmetric morphology and dismiss these processes because they cannot explain the point-symmetric morphology of Vela,the S-shaped high ejecta abundance pattern,and the enormous energy required to shape the S-shaped structure.Our findings strongly support the JJEM and further severely challenge the neutrino-driven explosion mechanism.展开更多
In this work,we apply tunneling formalism to analyze charged particles tunneling across a hairy black hole horizon.Such black hole solutions are essential for frameworks based on Horndeski's gravity theory.Applyin...In this work,we apply tunneling formalism to analyze charged particles tunneling across a hairy black hole horizon.Such black hole solutions are essential for frameworks based on Horndeski's gravity theory.Applying a semi-classical technique,we examine the tunneling of charged particles from a hairy black hole and derive the generic tunneling spectrum of released particles,ignoring self-gravitational and interaction.It is studied to ignore the back-reaction impact of the radiated particle on the hairy black hole.We analyze the properties of the black hole,such as temperature and entropy,under the influence of quantum gravity and also observe that the firstorder correction is present.We study tunneling radiation produced by a charged field equation in the presence of a generalized uncertainty effect.We modify the semi-classical technique by using the generalized uncertainty principle,the WKB approximation,and surface gravity.展开更多
The nature of progenitors of Type Ia supernovae(SNe Ia)and their explosion mechanism remains unclear.It has been suggested that SNe Ia may have resulted from thermonuclear explosions of hybrid carbon-oxygen-neon white...The nature of progenitors of Type Ia supernovae(SNe Ia)and their explosion mechanism remains unclear.It has been suggested that SNe Ia may have resulted from thermonuclear explosions of hybrid carbon-oxygen-neon white dwarfs(CONe WDs)when they grow in mass to approach the Chandrasekhar mass limit by accreting matter from a binary main-sequence(MS)companion.In this work,we combine the results of detailed binary evolution calculations with population synthesis models to investigate the rates and delay times of SNe Ia in the CONe WD+MS channel at a low metallicity environment of Z=0.0001.For a constant star formation rate of 5M_(⊙)yr^(−1),our calculations predict that the SN Ia rates in the CONe WD+MS channel at low metallicity of Z=0.0001 is about 0.11−3.89×10^(−4) yr^(−1).In addition,delay times in this channel cover a wide range of 0.05−2.5 Gyr.We further compare our results to those given by a previous study for the CONe WD+MS channel with a higher metallicity of Z=0.02 to explore the influence of metallicity on the results.We find that these two metallicity environments give a slight difference in rates and delay times of SNe Ia from the CONe WD+MS channel,although SNe Ia produced at a low metallicity environment of Z=0.0001 have relatively longer delay times.展开更多
We assume exponential corrections to the entropy of 5D charged Ad S black hole solutions,which are derived within the framework of Einstein-Gauss-Bonnet gravity and nonlinear electrodynamics.Additionally,we consider t...We assume exponential corrections to the entropy of 5D charged Ad S black hole solutions,which are derived within the framework of Einstein-Gauss-Bonnet gravity and nonlinear electrodynamics.Additionally,we consider two distinct versions of 5D charged Ad S black holes by setting the parameters q→0 and k→0(where q represents the charge,and k is the non-linear parameter).We investigate these black holes in the extended phase space,where the cosmological constant is interpreted as pressure,demonstrating the first law of black hole thermodynamics.The focus extends to understanding the thermal stability or instability,as well as identifying first and second-order phase transitions.This exploration is carried out through the analysis of various thermodynamic quantities,including heat capacity at constant pressure,Gibbs free energy(GFE),Helmholtz free energy(HFE),and the trace of the Hessian matrix.In order to visualize phase transitions,identify critical points,analyze stability and provide comprehensive analysis,we have made the contour plot of the mentioned thermodynamic quantities and observed that our results are very consistent.These investigations are conducted within the context of exponentially corrected entropies,providing valuable insights into the intricate thermodynamic behavior of these 5D charged Ad S black holes under different parameter limits.展开更多
We study the lensing phenomena of the strong gravity regime of five-dimensional charged,equally rotating black holes with a cosmological constant,familiarly known as the Cvetic–Lu–Pope(CLP)black holes.These black ho...We study the lensing phenomena of the strong gravity regime of five-dimensional charged,equally rotating black holes with a cosmological constant,familiarly known as the Cvetic–Lu–Pope(CLP)black holes.These black holes are characterized by three observable parameters,the mass M,the charge Q and the angular momentum J,in addition to the cosmological constant.We investigate the strong gravitational lensing observables,mainly the photon sphere radius,the minimum impact parameter,the deflection angle,the angular size,and the magnification of the relativistic images.We model the M87 and SgrA*for these observables.We also focus on the relativistic time delay effect in the strong-field regime of gravity and the impact of the observable on it.The analytical expressions for the observables of the relativistic images with vanishing angular momentum(j=0)are discussed in some detail.We shed a light on the gravitational time delay effect by incorporating the lensing observables.The gravitational time delay has a direct consequence on the photon sphere radius and hence on the quasinormal modes.展开更多
This study explores the dynamics of charged Hayward black holes,focusing on the effects of electric charge and the length factor on accretion disk characteristics.Our results show that increasing both parameters reduc...This study explores the dynamics of charged Hayward black holes,focusing on the effects of electric charge and the length factor on accretion disk characteristics.Our results show that increasing both parameters reduces the size of the event horizon and innermost stable circular orbits(ISCO)radius,with the electric charge exerting a more pronounced influence.Additionally,the length factor and electric charge can effectively replicate the spin of a Kerr black hole.Both parameters also affect the electromagnetic radiation emitted from the accretion disk,increasing the flux,temperature,and radiative efficiency.The peak radiation occurs in the soft x-ray band,with higher values of electric charge and length factor enhancing disk luminosity and shifting the peak to higher frequencies.These findings can offer valuable insights into the accretion processes around black holes and their observable signatures,particularly in x-ray astronomy.展开更多
In this article, our primary objective is to construct new wormhole solutions by involving a Yukawa-corrected form of Casimir energy density in a well-motivated gravitational theory that allows the coupling of curvatu...In this article, our primary objective is to construct new wormhole solutions by involving a Yukawa-corrected form of Casimir energy density in a well-motivated gravitational theory that allows the coupling of curvature and matter, namely the F(R,T) theory. To achieve this goal, a wormhole geometry exhibiting a spherically-symmetric nature is taken into account and anisotropic fluid is assumed to be the background ordinary matter source.We first consider the simple linear F(R,T) theory by assuming F(R,T) = R+ 2ζ T with L_m=-P(average pressure). Secondly, we utilize the conformal symmetries of the spherical-symmetric geometry for simplifying the resulting field equations and obtain the corresponding analytical form of the wormhole solution. In both cases, the viability of the proposed solutions is examined by checking the basic features of the wormhole shape model along with the validity of null energy constraints. Further, we study the volume integral quantifier(VIQ), exoticity factor and stability through the Tolman–Oppenheimer–Volkov(TOV) equation as well as the adiabatic index, active gravitational mass and complexity factor graphically. Lastly, we use a newly-proposed wormhole shape function to find the expressions of state variables and discuss the validity of energy bounds. We also explore the significance of this wormhole shape model through different quantities graphically. In all scenarios, the presented solutions are found to be new, promising and viable.展开更多
In this paper,we present the second post-Newtonian solution for the quasi-Keplerian motion of a test particle in the regular Simpson–Visser black-bounce spacetime which has a bounce parameter a.The obtained solution ...In this paper,we present the second post-Newtonian solution for the quasi-Keplerian motion of a test particle in the regular Simpson–Visser black-bounce spacetime which has a bounce parameter a.The obtained solution is formulated in terms of orbital energy,angular momentum,and the bounce parameter of the black hole.We explicitly analyze the leading effects of the bounce parameter which has dimensions of length,on the test particle’s orbit,including the periastron advance and orbital period.Then,we apply this model to the precessing motion of OJ 287 and determine the upper limits of the dimensionless bounce parameter as a/m=3.45±0.01,where m is the mass of the regular black hole.Compared with the bound given by the periastron advance of star S2,our bound on a/m is reduced by one order of magnitude,although our upper limit of a still needs further improvement.展开更多
The nearest GRB 170817A provided an opportunity to probe the angular structure of the jet of this short gamma-ray burst(SGRB),by using its off-axis observed afterglow emission.It is investigated whether the afterglow-...The nearest GRB 170817A provided an opportunity to probe the angular structure of the jet of this short gamma-ray burst(SGRB),by using its off-axis observed afterglow emission.It is investigated whether the afterglow-constrained jet structures can be consistent with the luminosity of the prompt emission of GRB 170817A.Furthermore,by assuming that all SGRBs,including GRB 170817A,have the same explosive mechanism and jet structure,we apply the different jet structures to the calculation of the flux and redshift distributions of the SGRB population,confronting them with the observational distributions of the Swift and Fermi sources.In comparison,it is found that the power-law and double-Gaussian models could be somewhat more favored than the single-Gaussian structure,as the last one could not be very consistent with the flux distribution of the Fermi data.Nevertheless,in view of the large uncertainty of parameters,we are still unable to make a suffciently conclusive judgement at present.展开更多
By regarding the Newton constant GNand cosmological constantΛas variables,in this paper we study the thermodynamics and phase transition of the Reissner-Nordstr o m anti-de Sitter(RN-Ad S)black hole with a global mon...By regarding the Newton constant GNand cosmological constantΛas variables,in this paper we study the thermodynamics and phase transition of the Reissner-Nordstr o m anti-de Sitter(RN-Ad S)black hole with a global monopole within the framework of Ad S/CFT correspondence.We find interesting critical phenomena and phase behavior in the(grand)canonical ensembles of fixed(Q,V,C),(Φ,V,C)and(Q,V,μ).When the other parameters are fixed,the free energy decreases with the global monopole increases.In the(Q,V,C)ensemble,the range of the unstable region decreases with the increase of the global monopole.In the(Φ,V,C)ensemble,whenΦ<Φc,the free energy appears as two branches,where the upper and lower branches correspond to low and high entropy,respectively.When(Q,V,μ)is fixed,a new zero-order phase transition occurs in the high-entropy phase and the low-entropy phase at certainμ-dependent temperatures.Whenμincreases to a certain value,this zero-order phase transition disappears.This certain value is negatively related to the magnitude of the global monopole.Finally,we find that p-V criticality does not appear with the change of global monopole.Therefore,it is important to note that the CFT states of charged black holes with global monopoles do not correspond to van der Waals fluids.Finally,we find that charged black holes with global monopoles can better reflect thermodynamic phase transitions and critical phenomena under the Ad S/CFT correspondence.By adjusting the change of the global monopole,the thermodynamic phase transition will also change.展开更多
We apply the WKB approximation method,matrix method,and finite difference method to study the gravitational quasi-normal modes of charged spherically symmetric black holes surrounded by quintessence fluid in Rastall g...We apply the WKB approximation method,matrix method,and finite difference method to study the gravitational quasi-normal modes of charged spherically symmetric black holes surrounded by quintessence fluid in Rastall gravity.By comparing the spherically symmetric spacetime metric of charged black holes surrounded by quintessence fluid in Rastall gravity with that of general relativity,we can find that the modifications to general relativity in this modified gravity theory can be described by parameters such asλ,Q,and C_(a),etc.In four-dimensional spacetime,we investigate the impact of charge Q and parameter C_(a) on the gravitational quasi-normal modes of charged black holes surrounded by quintessence field in Rastall gravity.The aim is to search for observational evidence of such black holes in astrophysical observations and,consequently,test the validity of Rastall theory.In five-dimensional(5D)spacetime,we study the impact of the parameter C_(a) on the gravitational quasi-normal modes of Rastall black holes surrounded by quintessence field and summarize the corresponding variation patterns.展开更多
The QCD axion bubbles can form due to an explicit breaking of the Peccei–Quinn symmetry in the early Universe.In this paper,we investigate the modified formation of a QCD axion bubble in the presence of an axionlike ...The QCD axion bubbles can form due to an explicit breaking of the Peccei–Quinn symmetry in the early Universe.In this paper,we investigate the modified formation of a QCD axion bubble in the presence of an axionlike particle(ALP),considering its resonant conversion to a QCD axion.We consider a general scenario where the QCD axion mixes with ALP before the QCD phase transition.In this scenario,the energy density of the ALP can be adiabatically transferred to the QCD axion at a temperature T_(R),resulting in the suppression of the cosmic background temperature T_(B)at which the energy density of the QCD axion equals that of the radiation.The QCD axion bubbles form when the QCD axions arise during the QCD phase transition.Finally,we briefly discuss the impact of the formation of QCD axion bubbles on the formation of primordial black holes.展开更多
The effects and rules of the dimensionless parameterξon neutrino annihilation v+v→e^(-)+e^(+)dominated gamma-ray bursts are analysed and investigated within the context of black holes in asymptotic safety.We also co...The effects and rules of the dimensionless parameterξon neutrino annihilation v+v→e^(-)+e^(+)dominated gamma-ray bursts are analysed and investigated within the context of black holes in asymptotic safety.We also computationally model photon orbits around black holes,as photons and neutrinos have the same geodesic equations near black holes.We show that the black hole shadow radius decreases with increasingξ.Calculations are made to determine the temperature of the accretion disk surrounding the black hole and the ratio Q/Q_(Newt)of energy deposition per unit time and compared to that of the Newtonian scenario.The accretion disk temperature peaks at a higher temperature due to quantum gravity corrections,which increases the probability of neutrino emission from the black hole.It is interesting to note that larger quantum gravity effects cause the ratio value to significantly decline.In the neutrinoantineutrino annihilation process,the energy deposition rate is sufficient even while the energy conversion is inhibited because of quantum corrections.Gamma-ray bursts might originate from the corrected annihilation process.Additionally,we examine the derivative dQ/dr about the star radius r.The findings demonstrate that the ratio is lowered by the black hole's quantum influence.The neutrino pair annihilation grows weaker the more prominent the influence of quantum gravity.展开更多
基金A grant from the Pazy Foundation supported this research
文摘We identify an S-shaped main-jet axis in the Vela core-collapse supernova remnant(CCSNR)that we attribute to a pair of precessing jets,one of the tens of pairs of jets that exploded the progenitor of Vela according to the jittering jets explosion mechanism(JJEM).A main-jet axis is a symmetry axis across the CCSNR and through the center.We identify the S-shaped main-jet axis by the high abundance of ejecta elements,oxygen,neon,and magnesium.We bring the number of identified pairs of clumps and ears in Vela to seven,two pairs shaped by the pair of precessing jets that formed the main-jet axis.The pairs and the main-jet axis form the point-symmetric wind-rose structure of Vela.The other five pairs of clumps/ears do not have signatures near the center,only on two opposite sides of the CCSNR.We discuss different possible jet-less shaping mechanisms to form such a point-symmetric morphology and dismiss these processes because they cannot explain the point-symmetric morphology of Vela,the S-shaped high ejecta abundance pattern,and the enormous energy required to shape the S-shaped structure.Our findings strongly support the JJEM and further severely challenge the neutrino-driven explosion mechanism.
基金funded by the National Natural Science Foundation of China under Grant No.11975145。
文摘In this work,we apply tunneling formalism to analyze charged particles tunneling across a hairy black hole horizon.Such black hole solutions are essential for frameworks based on Horndeski's gravity theory.Applying a semi-classical technique,we examine the tunneling of charged particles from a hairy black hole and derive the generic tunneling spectrum of released particles,ignoring self-gravitational and interaction.It is studied to ignore the back-reaction impact of the radiated particle on the hairy black hole.We analyze the properties of the black hole,such as temperature and entropy,under the influence of quantum gravity and also observe that the firstorder correction is present.We study tunneling radiation produced by a charged field equation in the presence of a generalized uncertainty effect.We modify the semi-classical technique by using the generalized uncertainty principle,the WKB approximation,and surface gravity.
基金supported by the Strategic Priority Research Program of the Chinese Academy of Sciences(grant Nos.XDB1160303,XDB1160000)the National Natural Science Foundation of China(NSFC,Nos.12288102,12333008,12090040/1,11873016,11973080,and 11803030)+3 种基金the National Key R&D Program of China(Nos.2021YFA1600403,2021YFA1600401 and 2021YFA1600400)the Chinese Academy of Sciences(CAS),the Yunnan Ten Thousand Talents Plan–Young&Elite Talents Project,and the CAS“Light of West China”Program,the International Centre of Supernovae,Yunnan Key Laboratory(No.202302AN360001)the Yunnan Fundamental Research Projects(grant Nos.202401BC070007,202201BC070003,and 202001AW070007)the“Yunnan Revitalization Talent Support Program”—Science&Technology Champion Project and Yunling Scholar Project(No.202305AB350003).
文摘The nature of progenitors of Type Ia supernovae(SNe Ia)and their explosion mechanism remains unclear.It has been suggested that SNe Ia may have resulted from thermonuclear explosions of hybrid carbon-oxygen-neon white dwarfs(CONe WDs)when they grow in mass to approach the Chandrasekhar mass limit by accreting matter from a binary main-sequence(MS)companion.In this work,we combine the results of detailed binary evolution calculations with population synthesis models to investigate the rates and delay times of SNe Ia in the CONe WD+MS channel at a low metallicity environment of Z=0.0001.For a constant star formation rate of 5M_(⊙)yr^(−1),our calculations predict that the SN Ia rates in the CONe WD+MS channel at low metallicity of Z=0.0001 is about 0.11−3.89×10^(−4) yr^(−1).In addition,delay times in this channel cover a wide range of 0.05−2.5 Gyr.We further compare our results to those given by a previous study for the CONe WD+MS channel with a higher metallicity of Z=0.02 to explore the influence of metallicity on the results.We find that these two metallicity environments give a slight difference in rates and delay times of SNe Ia from the CONe WD+MS channel,although SNe Ia produced at a low metallicity environment of Z=0.0001 have relatively longer delay times.
基金the Deanship of Research and Graduate Studies at King Khalid University for funding this work through Large Research Project under Grant No.RGP2/539/45。
文摘We assume exponential corrections to the entropy of 5D charged Ad S black hole solutions,which are derived within the framework of Einstein-Gauss-Bonnet gravity and nonlinear electrodynamics.Additionally,we consider two distinct versions of 5D charged Ad S black holes by setting the parameters q→0 and k→0(where q represents the charge,and k is the non-linear parameter).We investigate these black holes in the extended phase space,where the cosmological constant is interpreted as pressure,demonstrating the first law of black hole thermodynamics.The focus extends to understanding the thermal stability or instability,as well as identifying first and second-order phase transitions.This exploration is carried out through the analysis of various thermodynamic quantities,including heat capacity at constant pressure,Gibbs free energy(GFE),Helmholtz free energy(HFE),and the trace of the Hessian matrix.In order to visualize phase transitions,identify critical points,analyze stability and provide comprehensive analysis,we have made the contour plot of the mentioned thermodynamic quantities and observed that our results are very consistent.These investigations are conducted within the context of exponentially corrected entropies,providing valuable insights into the intricate thermodynamic behavior of these 5D charged Ad S black holes under different parameter limits.
基金supported by the National Natural Science Foundation of China under Grants Nos.12475056,12347177,and 12247101,the 111 Project under Grant No.B20063Lanzhou City's scientific research funding subsidy to Lanzhou Universitythe Gansu Province Major Scientific and Technological Special Project。
文摘We study the lensing phenomena of the strong gravity regime of five-dimensional charged,equally rotating black holes with a cosmological constant,familiarly known as the Cvetic–Lu–Pope(CLP)black holes.These black holes are characterized by three observable parameters,the mass M,the charge Q and the angular momentum J,in addition to the cosmological constant.We investigate the strong gravitational lensing observables,mainly the photon sphere radius,the minimum impact parameter,the deflection angle,the angular size,and the magnification of the relativistic images.We model the M87 and SgrA*for these observables.We also focus on the relativistic time delay effect in the strong-field regime of gravity and the impact of the observable on it.The analytical expressions for the observables of the relativistic images with vanishing angular momentum(j=0)are discussed in some detail.We shed a light on the gravitational time delay effect by incorporating the lensing observables.The gravitational time delay has a direct consequence on the photon sphere radius and hence on the quasinormal modes.
文摘This study explores the dynamics of charged Hayward black holes,focusing on the effects of electric charge and the length factor on accretion disk characteristics.Our results show that increasing both parameters reduces the size of the event horizon and innermost stable circular orbits(ISCO)radius,with the electric charge exerting a more pronounced influence.Additionally,the length factor and electric charge can effectively replicate the spin of a Kerr black hole.Both parameters also affect the electromagnetic radiation emitted from the accretion disk,increasing the flux,temperature,and radiative efficiency.The peak radiation occurs in the soft x-ray band,with higher values of electric charge and length factor enhancing disk luminosity and shifting the peak to higher frequencies.These findings can offer valuable insights into the accretion processes around black holes and their observable signatures,particularly in x-ray astronomy.
文摘In this article, our primary objective is to construct new wormhole solutions by involving a Yukawa-corrected form of Casimir energy density in a well-motivated gravitational theory that allows the coupling of curvature and matter, namely the F(R,T) theory. To achieve this goal, a wormhole geometry exhibiting a spherically-symmetric nature is taken into account and anisotropic fluid is assumed to be the background ordinary matter source.We first consider the simple linear F(R,T) theory by assuming F(R,T) = R+ 2ζ T with L_m=-P(average pressure). Secondly, we utilize the conformal symmetries of the spherical-symmetric geometry for simplifying the resulting field equations and obtain the corresponding analytical form of the wormhole solution. In both cases, the viability of the proposed solutions is examined by checking the basic features of the wormhole shape model along with the validity of null energy constraints. Further, we study the volume integral quantifier(VIQ), exoticity factor and stability through the Tolman–Oppenheimer–Volkov(TOV) equation as well as the adiabatic index, active gravitational mass and complexity factor graphically. Lastly, we use a newly-proposed wormhole shape function to find the expressions of state variables and discuss the validity of energy bounds. We also explore the significance of this wormhole shape model through different quantities graphically. In all scenarios, the presented solutions are found to be new, promising and viable.
基金supported by the National Natural Science Foundation of China(Grant Nos.12303079,12481540180 and 12475057)the support of the postdoctoral program of purple Mountain Observatory,Chinese Academy of Sciences。
文摘In this paper,we present the second post-Newtonian solution for the quasi-Keplerian motion of a test particle in the regular Simpson–Visser black-bounce spacetime which has a bounce parameter a.The obtained solution is formulated in terms of orbital energy,angular momentum,and the bounce parameter of the black hole.We explicitly analyze the leading effects of the bounce parameter which has dimensions of length,on the test particle’s orbit,including the periastron advance and orbital period.Then,we apply this model to the precessing motion of OJ 287 and determine the upper limits of the dimensionless bounce parameter as a/m=3.45±0.01,where m is the mass of the regular black hole.Compared with the bound given by the periastron advance of star S2,our bound on a/m is reduced by one order of magnitude,although our upper limit of a still needs further improvement.
基金supported by the National Key R&D Program of China(2021YFA0718500)the China Manned Spaced Project(CMS-CSST-2021-A12)+1 种基金the National Natural Science Foundation of China(grant Nos.12393811,U1838203,and11803007)Hubei Provincial Outstanding Young and Middle-aged Science and Technology Innovation Team Project of China(T2021026)。
文摘The nearest GRB 170817A provided an opportunity to probe the angular structure of the jet of this short gamma-ray burst(SGRB),by using its off-axis observed afterglow emission.It is investigated whether the afterglow-constrained jet structures can be consistent with the luminosity of the prompt emission of GRB 170817A.Furthermore,by assuming that all SGRBs,including GRB 170817A,have the same explosive mechanism and jet structure,we apply the different jet structures to the calculation of the flux and redshift distributions of the SGRB population,confronting them with the observational distributions of the Swift and Fermi sources.In comparison,it is found that the power-law and double-Gaussian models could be somewhat more favored than the single-Gaussian structure,as the last one could not be very consistent with the flux distribution of the Fermi data.Nevertheless,in view of the large uncertainty of parameters,we are still unable to make a suffciently conclusive judgement at present.
基金supported by the Natural Science Foundation of Sichuan Province(Grant No.2022NSFSC1833)the Sichuan Science and Technology Program(Grant No.2023ZYD0023)the Science Technology Department of Sichuan Province(Grant No.R21ZYZF0001)。
文摘By regarding the Newton constant GNand cosmological constantΛas variables,in this paper we study the thermodynamics and phase transition of the Reissner-Nordstr o m anti-de Sitter(RN-Ad S)black hole with a global monopole within the framework of Ad S/CFT correspondence.We find interesting critical phenomena and phase behavior in the(grand)canonical ensembles of fixed(Q,V,C),(Φ,V,C)and(Q,V,μ).When the other parameters are fixed,the free energy decreases with the global monopole increases.In the(Q,V,C)ensemble,the range of the unstable region decreases with the increase of the global monopole.In the(Φ,V,C)ensemble,whenΦ<Φc,the free energy appears as two branches,where the upper and lower branches correspond to low and high entropy,respectively.When(Q,V,μ)is fixed,a new zero-order phase transition occurs in the high-entropy phase and the low-entropy phase at certainμ-dependent temperatures.Whenμincreases to a certain value,this zero-order phase transition disappears.This certain value is negatively related to the magnitude of the global monopole.Finally,we find that p-V criticality does not appear with the change of global monopole.Therefore,it is important to note that the CFT states of charged black holes with global monopoles do not correspond to van der Waals fluids.Finally,we find that charged black holes with global monopoles can better reflect thermodynamic phase transitions and critical phenomena under the Ad S/CFT correspondence.By adjusting the change of the global monopole,the thermodynamic phase transition will also change.
基金Project supported by the National Natural Science Foundation of China(Grant No.42230207)the Fundamental Research Funds for the Central Universities,China University of Geosciences(Wuhan)(Grant No.G1323523064)。
文摘We apply the WKB approximation method,matrix method,and finite difference method to study the gravitational quasi-normal modes of charged spherically symmetric black holes surrounded by quintessence fluid in Rastall gravity.By comparing the spherically symmetric spacetime metric of charged black holes surrounded by quintessence fluid in Rastall gravity with that of general relativity,we can find that the modifications to general relativity in this modified gravity theory can be described by parameters such asλ,Q,and C_(a),etc.In four-dimensional spacetime,we investigate the impact of charge Q and parameter C_(a) on the gravitational quasi-normal modes of charged black holes surrounded by quintessence field in Rastall gravity.The aim is to search for observational evidence of such black holes in astrophysical observations and,consequently,test the validity of Rastall theory.In five-dimensional(5D)spacetime,we study the impact of the parameter C_(a) on the gravitational quasi-normal modes of Rastall black holes surrounded by quintessence field and summarize the corresponding variation patterns.
基金partly supported by the National Natural Science Foundation of China(NSFC)(Grants No.11775025 and No.12175027)partly supported by the Key Laboratory of Theoretical Physics in the Institute of Theoretical PhysicsCAS。
文摘The QCD axion bubbles can form due to an explicit breaking of the Peccei–Quinn symmetry in the early Universe.In this paper,we investigate the modified formation of a QCD axion bubble in the presence of an axionlike particle(ALP),considering its resonant conversion to a QCD axion.We consider a general scenario where the QCD axion mixes with ALP before the QCD phase transition.In this scenario,the energy density of the ALP can be adiabatically transferred to the QCD axion at a temperature T_(R),resulting in the suppression of the cosmic background temperature T_(B)at which the energy density of the QCD axion equals that of the radiation.The QCD axion bubbles form when the QCD axions arise during the QCD phase transition.Finally,we briefly discuss the impact of the formation of QCD axion bubbles on the formation of primordial black holes.
基金partly supported by the Shanghai Key Laboratory of Astrophysics 18DZ2271600。
文摘The effects and rules of the dimensionless parameterξon neutrino annihilation v+v→e^(-)+e^(+)dominated gamma-ray bursts are analysed and investigated within the context of black holes in asymptotic safety.We also computationally model photon orbits around black holes,as photons and neutrinos have the same geodesic equations near black holes.We show that the black hole shadow radius decreases with increasingξ.Calculations are made to determine the temperature of the accretion disk surrounding the black hole and the ratio Q/Q_(Newt)of energy deposition per unit time and compared to that of the Newtonian scenario.The accretion disk temperature peaks at a higher temperature due to quantum gravity corrections,which increases the probability of neutrino emission from the black hole.It is interesting to note that larger quantum gravity effects cause the ratio value to significantly decline.In the neutrinoantineutrino annihilation process,the energy deposition rate is sufficient even while the energy conversion is inhibited because of quantum corrections.Gamma-ray bursts might originate from the corrected annihilation process.Additionally,we examine the derivative dQ/dr about the star radius r.The findings demonstrate that the ratio is lowered by the black hole's quantum influence.The neutrino pair annihilation grows weaker the more prominent the influence of quantum gravity.
