Quantum Fisher information(QFI)associated with local metrology has been used to parameter estimation in open quantum systems.In this work,we calculated the QFI for a moving Unruh-DeWitt detector coupled with massless ...Quantum Fisher information(QFI)associated with local metrology has been used to parameter estimation in open quantum systems.In this work,we calculated the QFI for a moving Unruh-DeWitt detector coupled with massless scalar fields in n-dimensional spacetime,and analyzed the behavior of QFI with various parameters,such as the dimension of spacetime,evolution time,and Unruh temperature.We discovered that the QFI of state parameter decreases monotonically from 1 to 0 over time.Additionally,we noted that the QFI for small evolution times is several orders of magnitude higher than the QFI for long evolution times.We also found that the value of QFI decreases at first and then stabilizes as the Unruh temperature increases.It was observed that the QFI depends on initial state parameterθ,and Fθis the maximum forθ=0 orθ=π,Fφis the maximum forθ=π/2.We also obtain that the maximum value of QFI for state parameters varies for different spacetime dimensions with the same evolution time.展开更多
本文求出了共形标量因子梯度与流体四速度垂直时的有切无旋CRFPEF流体Einstein-Maxwell方程严格解,指出有两种可能类型:(1)共形平直解;(2)与在类时超曲面上具有三维运动群的BianchiVI_0型真空解共形.在电磁场为0的特殊情况下,本结果为...本文求出了共形标量因子梯度与流体四速度垂直时的有切无旋CRFPEF流体Einstein-Maxwell方程严格解,指出有两种可能类型:(1)共形平直解;(2)与在类时超曲面上具有三维运动群的BianchiVI_0型真空解共形.在电磁场为0的特殊情况下,本结果为有切无旋Van den Bergh解.展开更多
This paper investigates the resonant frequencies of the massless scalar field in the near extremal Kerr-like black-brane spacetime. It is shown that the different angular quantum number will present different resonant...This paper investigates the resonant frequencies of the massless scalar field in the near extremal Kerr-like black-brane spacetime. It is shown that the different angular quantum number will present different resonant frequencies. It is also shown that the real part of the resonant frequencies increases as the compact dimensions parameter μi increases, but the magnitude of the imaginary part decreases as μi increases.展开更多
The intermediate asymptotic quasinormal mode spectrum of the charged scalar and Dirac fields in the near extremal Kerr-Newman black hole is studied analytically, It is found that the quasinormal mode spectrum can be e...The intermediate asymptotic quasinormal mode spectrum of the charged scalar and Dirac fields in the near extremal Kerr-Newman black hole is studied analytically, It is found that the quasinormal mode spectrum can be expressed in terms of the Hawking temperature Thb, the electric potential Ф＋ and the horizon＇s angular velocity ΩH for the case of （eФ_ ＋ mΩH） 〉 （1 - 4πThb）Re（ω） （where e is the charge and m is the azimuthal projection number）, whereas it is only relevant to the charge and the mass parameter for another case. It is also shown that by using the Bohr＇s correspondence principle, the fundamental change in the black-hole surface area induced by the emission of a rotating charged quantum from the Kerr-Newman black hole is in accord with the Bekenstein-Mukhanov general prediction.展开更多
By using the third-order Wentzel-Kramers-Brillouin approximation and the monodromy methods, the quasnormal modes of a coupled scalar field in the canonical non-rotating acoustic black hole spacetime are investigated. ...By using the third-order Wentzel-Kramers-Brillouin approximation and the monodromy methods, the quasnormal modes of a coupled scalar field in the canonical non-rotating acoustic black hole spacetime are investigated. It is shown that the coupling between the scalar field and background metric affects the quasinormal frequencies. At low overtones, both the real part and the magnitude of imaginary part increase with the couple factor ξ. For the larger ξ, both of them are almost linearly related to the couple factor. At high overtones, it is found that the frequency formula of the quasinormal modes is 2πω/κ = ln （ 1 ＋ 2 cos√9-24ξ/5 π） - i（2n ＋ 1）π, which means that 5 when ξ is larger, the real part is the linear function of ξ^1/2.展开更多
基金Project supported by the National Natural Science Foundation of China(Grant Nos.12105097 and 12035005)the Science Research Fund of the Education Department of Hunan Province,China(Grant No.23B0480).
文摘Quantum Fisher information(QFI)associated with local metrology has been used to parameter estimation in open quantum systems.In this work,we calculated the QFI for a moving Unruh-DeWitt detector coupled with massless scalar fields in n-dimensional spacetime,and analyzed the behavior of QFI with various parameters,such as the dimension of spacetime,evolution time,and Unruh temperature.We discovered that the QFI of state parameter decreases monotonically from 1 to 0 over time.Additionally,we noted that the QFI for small evolution times is several orders of magnitude higher than the QFI for long evolution times.We also found that the value of QFI decreases at first and then stabilizes as the Unruh temperature increases.It was observed that the QFI depends on initial state parameterθ,and Fθis the maximum forθ=0 orθ=π,Fφis the maximum forθ=π/2.We also obtain that the maximum value of QFI for state parameters varies for different spacetime dimensions with the same evolution time.
文摘本文求出了共形标量因子梯度与流体四速度垂直时的有切无旋CRFPEF流体Einstein-Maxwell方程严格解,指出有两种可能类型:(1)共形平直解;(2)与在类时超曲面上具有三维运动群的BianchiVI_0型真空解共形.在电磁场为0的特殊情况下,本结果为有切无旋Van den Bergh解.
基金Project supported by the National Natural Science Foundation of China (Grant No 10675045)the Foundation for the Author of National Excellent Doctoral Dissertation of China (Grant No 200317)
文摘This paper investigates the resonant frequencies of the massless scalar field in the near extremal Kerr-like black-brane spacetime. It is shown that the different angular quantum number will present different resonant frequencies. It is also shown that the real part of the resonant frequencies increases as the compact dimensions parameter μi increases, but the magnitude of the imaginary part decreases as μi increases.
基金Supported by the National Natural Science Foundation of China under Grant No 10675045, the Foundation for the Author of National Excellent Doctoral Dissertation of China under Grant No 200317, the Hunan Provincial Natural Science Foundation of China under Grant No 07A0128, and the Construct Programme of the Key Discipline in Hunan Province.
文摘The intermediate asymptotic quasinormal mode spectrum of the charged scalar and Dirac fields in the near extremal Kerr-Newman black hole is studied analytically, It is found that the quasinormal mode spectrum can be expressed in terms of the Hawking temperature Thb, the electric potential Ф＋ and the horizon＇s angular velocity ΩH for the case of （eФ_ ＋ mΩH） 〉 （1 - 4πThb）Re（ω） （where e is the charge and m is the azimuthal projection number）, whereas it is only relevant to the charge and the mass parameter for another case. It is also shown that by using the Bohr＇s correspondence principle, the fundamental change in the black-hole surface area induced by the emission of a rotating charged quantum from the Kerr-Newman black hole is in accord with the Bekenstein-Mukhanov general prediction.
基金Supported by the FANEDD under Grant No 2003052, the Natural Science Foundation of Hunan Province of China under Grant No 05JJ40012 and the Hunan Normal University Natural Science Foundation under Grant No 22040639.
文摘By using the third-order Wentzel-Kramers-Brillouin approximation and the monodromy methods, the quasnormal modes of a coupled scalar field in the canonical non-rotating acoustic black hole spacetime are investigated. It is shown that the coupling between the scalar field and background metric affects the quasinormal frequencies. At low overtones, both the real part and the magnitude of imaginary part increase with the couple factor ξ. For the larger ξ, both of them are almost linearly related to the couple factor. At high overtones, it is found that the frequency formula of the quasinormal modes is 2πω/κ = ln （ 1 ＋ 2 cos√9-24ξ/5 π） - i（2n ＋ 1）π, which means that 5 when ξ is larger, the real part is the linear function of ξ^1/2.
