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1811.06947.Pdf Kinetic Spin Decoherence in a Gravitational Field Yue Dai∗ Beijing Computational Science Research Center, Beijing 100193, China Yu Shi† Department of Physics & State Key Laboratory of Surface Physics, Fudan University, Shanghai 200433, China and Collaborative Innovation Center of Advanced Microstructures, Fudan University, Shanghai 200433, China Abstract We consider a wave packet of a spin-1/2 particle in a gravitational field, the effect of which can be described in terms of a succession of local inertial frames. It is shown that integrating out of the momentum yields a spin mixed state, with the entropy dependent on the deviation of metric from the flat spacetime. The decoherence occurs even if the particle is static in the gravitational field. arXiv:1811.06947v1 [gr-qc] 16 Nov 2018 1 Spacetime tells matter how to move [1]. For quantum objects, spacetime tells quantum states how to evolve, that is, the quantum states are affected by the gravitational field. For example, by considering quantum fields near black holes, Hawking showed that black holes emit thermal particles [2, 3]. Analogously, Unruh showed that an accelerated detector in the Minkowski vacuum detects thermal radiation [4, 5]. In recent years, there have been a large number of discussions about quantum decoherence and quantum entanglement degradation in quantum fields [6–14]. On the other hand, decoherence in the spin state due to the change of reference frame exists also for a single relativistic particle with spin degree of freedom. It was shown that the spin entropy is not invariant under Lorentz transformation unless the particle is in a momentum eigenstate [15]. Such an effect can be generalized to the presence of a gravitational field, by considering a continuous succession of Lorentz transformations. This is a kinetic way of decoherence, and occurs even if the particle is static. It has been shown, for a particle moving around a black hole near the Schwarzschild horizon, that a rapid spin decoherence is observed for an observer static in the Killing time [16]. EPR correlation and the violation of Bell inequality were also investigated [17]. In this Letter, we show that spin decoherence is quite general for a particle in a gravitational field even if the particle is static. µ The state Ψp,σ of a massive particle is the eigenvector of the four-momentum p , and σ denotes the spin. Under a homogeneous Lorentz transformation Λ which carries the µ µ µ ν momentum from p to q =Λ νp , the state of the particle transforms as [18] 0 (Λp) (1/2) ′ ′ U(Λ)Ψp,σ = 0 Dσ σ (W (Λ,p))ΨΛp,σ , (1) s p ′ Xσ 1/2 where Dσ′σ(W (Λ,p)) is the spin-1/2 representation of the Wigner rotaion W (Λ,p) = 1 L− (Λp)ΛL(p), where L(p) represents a “standard boost” that carries the momentum from (m, 0, 0, 0) to pµ and can be chosen as pµ [L(p)]µ = [L(p)]0 = , (2) 0 µ m pip [L(p)]i = δi + j , (3) j j m(p0 + m) where m is the mass of the particle, and indices i, j = 1, 2, 3. It can be calculated that 0 i 0 W 0 = 1, W 0 = W i = 0, and Λi p qiΛ0 W i =Λi + 0 j j . (4) j j p0 + m − q0 + m 2 Now we calculate the Wigner rotation of a massive spin-1/2 particle moving in the grav- itational field. Consider the spacetime metric ds2 = (1 + gx)2dt2 + dx2 + dy2 + dz2, (5) − which corresponds to the local coordinate system of an accelerated observer in flat spacetime or an observer in a uniform gravitational field [1]. It can also characterize the spacetime near the event horizon of a Schwarzschild black hole, as the near horizon spacetime is locally flat for a large black hole, and static observers near the horizon in the Schwarzschild spacetime correspond to accelerated observers in Minkowski spacetime [19, 20]. We assume that the particle is moving with constant velocity uµ = dxµ/dτ, that is, the spatial components of the velocity are independent of time. Note that the particle is not in free fall, it must be subject to a force, which may cause spin decoherence dynamically. We avoid this dynamical effect by assuming that the particle does not experience any torque. In order to calculate the Wigner rotation, we introduce local inertial frames (LIF) at each µ spacetime point along the particle’s world line, by using a tetrad ea (x), defined through µ ν ea (x)eb (x)gµν (x)= ηab, (6) where we use Greek letters to label the general-coordinates (t, x, y, z), and Latin letters to label the coordinates of the LIF, with the components denoted as 0, 1, 2, 3. For given gµν(x), the locally inertial coordinate at x can only be determined up to order (x x )2, as a LIF 0 − 0 remains inertial after a Lorentz transformation [21]. But the spin entropy is not invariant between different LIFs. One choice of the LIF can be made by choosing 1 e t = , e x = e y = e z =1, (7) 0 1+ gx 1 2 3 and all the other components are zero. In this LIF, the magnitudes of the spatial components of velocity of the particle are the same as those in the general coordinate, thus we may exclude the special relativistic effects described in [15]. The inverse of the tetrad can be obtained from a ν ν a µ a e µ(x)ea (x)= δµ , e µ(x)eb (x)= δ b. (8) And any vector Aµ is transformed to a a µ A = e µA (9) 3 in the LIF. Now, if the particle does not move along a geodesic, the LIF updates with time, a a a a b so does the momentum of the particle p . The change of p can be written as δp = λ bp dη, a a a a a where η is the coordinate time of the LIF, and λ b is related to Λ b as Λ b = λ bdη + δ b. a λ b can be calculated to be λa = (aau uaa )+ χa , (10) b − b − b b where the first term is due to the acceleration of the particle, aa and ua are the acceleration a a µ and velocity in the LIF, respectively. a = e µa , where aµ = uν uµ = uν [∂ uµ +Γµ uσ] , (11) ∇ν ν νσ µ with Γ νσ being the Christoffel symbols, which can be calculated according to the standard procedures, and aa can be obtained by lowering the indices. The results are gux√1+ u2 a0 = a = , (12) − 0 1+ gx g(1 + u2) a1 = a = , (13) 1 1+ gx 2 3 a = a2 =0, a = a3 =0. (14) The components of velocity in the LIF are u0 = u = √1+ u2, (15) − 0 1 2 3 u = u1 = ux, u = u2 = uy, u = u3 = uz. (16) a The second term of Eq. (10), χ b, which characterizes the change of the LIF along the world line, is given by χa = uµ(x)[e ν(x) ea (x)] . (17) b b ∇µ ν a a Thus λ b and Λ b can be obtained. i Now we write W j as i i i W j = δ j + ω j, (18) and then, by using Eq. (4) with q0 = p0 in our case, we obtain 2 2 1 2 gpy m + p ω 2 = ω 1 = 2 , (19) − − (1p + gx)m 2 2 1 3 gpz m + p ω 3 = ω 1 = 2 , (20) − − (1p + gx)m 4 ω2 = ω3 =0, (21) 3 − 2 2 2 2 where p = px + py + pz. Note that ω’s depend on x, which in turn depend on px. For a wave packet,px may also has certain distribution, and we can simply replace x asx ¯ and the initial coordinatex ¯ of the center of the wave packet, since it can be shown that if we take into account the width of the wave packet in x direction, the difference is only of higher order. The spin-1/2 representation of the Winger rotation is 1/2 i D ′ (W (x)) = I + [ω (x)σ + ω (x)σ + ω σ ] dη σ σ 2 23 x 31 y 12 z i i = I + [ω(x) σ] dη = I + ω(x)(nˆ σ)dη, (22) 2 · 2 · 2 2 2 where ω(x)= ω12(x)+ ω23(x)+ ω31(x),n ˆi = ǫijkωjk(x)/ω(x), ǫijk is the completely antisym- i metric tensor with ǫ123 = 1, and nˆ =n ˆixˆ . For finite time η, η 1/2 i D ′ (η)= T exp ω(x)(nˆ σ)dη , (23) σ σ 2 · Z0 where T represents time ordering. Hence 1/2 θ θ D ′ (η)= I cos + i(nˆ σ) sin , (24) σ σ 2 · 2 where η θ = ω(x)dη Z0 2 2 2 2 2 2 2 gη p + p m + p gη px p + p y z y z , (25) ≈ 1+ gx¯ m2 − 1+ gx¯ 2m2 p p p For a spin-1/2 particle, the initial state a0(p) . b0(p) becomes a(p) 1/2 a0(p) = D ′ (η) (26) σ σ b(p) b0(p) after the Wigner rotation. Now we assume the initial wave packet is Gaussian, 2 − 2 2 3/4 1 (px−p¯x) (py p¯y) (pz−p¯z) π− 2 + 2 + 2 − 2 wx wy wz a0(p)= α e , (27) √wxwywz 5 2 − 2 2 3/4 1 (px−p¯x) (py p¯y) (pz−p¯z) π− 2 + 2 + 2 − 2 wx wy wz b0(p)= β e , (28) √wxwywz with α 2 + β 2 = 1, p¯ being the average momentum, and w being the width of the wave | | | | i i packet in each directions in the momentum space.
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