Decoherence of Higher Order Orbital Angular Momentum Entangled State in Non-Kolmogorov Turbulence

Abstract

The decay of OAM entanglement in non-Kolmogorov turbulence has been numerically evaluated. In this work, we explore the evolution of OAM entanglement with higher-order OAM mode in the weak scintillation regime. In particular, the results of the numerical evaluation show that the OAM entanglement state with higher value of the azimuthal mode and larger radial quantum number survives over a longer distance. Meanwhile, the beam parameters and turbulence parameters usually have significant influences on OAM entanglement. In addition, it is demonstrated that the effect of turbulence on the OAM entanglement is the most serious when the generalized exponent is around 3.07.

1. Introduction

Orbital angular momentum (OAM) photons have gained more and more attention in recent years. The orbital angular momentum (OAM) eigenstates of photons form an infinite-dimensional system, providing larger storage capacity and a number of potential benefits for quantum information purposes [1,2,3,4,5], which make them promising candidates for higher dimensional quantum key distribution [6].

Quantum entanglement is an essential physical resource, which can be applied significantly in the field of quantum information processing [7,8] but is highly fragile to the environment [9]. Recently, an enormous number of theoretical and experimental studies have been devoted to the turbulence-induced decay of OAM entanglement [9,10,11,12,13,14,15,16,17,18,19,20,21]. Nonetheless, it is still difficult to describe the behavior of OAM photons in turbulence. It is known that OAM-entangled photonic states are encoded in finite-dimensional Hilbert spaces. While OAM-entangled photons go through atmospheric turbulence, the scintillation process distorts the photons’ wave fronts and makes OAM modes spread throughout the entire Hilbert space [22]. In practice, however, only the information of the output states contained in the finite-dimensional encoding subspace can be extracted. As a consequence, it is essential to truncate the Hilbert space and calculate the truncated density matrix for predicting OAM entanglement evolution. The truncated density matrix can obtain the scattering to density matrix elements from outside the subspace, but the effect of backward scattering from the outside subspace to elements in the subspace is always lost [20]. However, when the coupling of states between inside the encoding subspace and outside is strong, the truncation of the Hilbert space unavoidably leads to a decay of the output state’s norm [23], and the backward scattering is particularly important to higher-order OAM modes [24]. Moreover, most previous theoretical studies on the effects of atmospheric turbulence on OAM entanglement have always considered the entangled OAM states with a zero radial index [14,15,16,17,18,19,20], but the entanglement decoherence of OAM photons with non-zero radial index has seldom been mentioned.

In the present contribution, the OAM-entangled two-photon state’s propagation through a non-Kolmogorov turbulent atmosphere has been numerically evaluated. We consider that the evolution of the OAM entanglement is in the weak scintillation regime. Therefore, the turbulence-caused intensity scintillation is ignored. Here, we significantly focus on the evolution of OAM entanglement with higher-order OAM mode in turbulence when the backward scattering is taken into account. In addition, Wootter’s concurrence is introduced to quantify the OAM entanglement [25]. The rest of the paper is organized as follows: In Section 2, the numerical procedure will be introduced, while the results of numerical evaluation and its analysis will be provided in Section 3. The discussion and conclusions are presented and provided in Section 4.

2. Numerical Procedure

The quantum communication system is presented in Figure 1. A pair of entangled photons are emitted by the source field. Initially, it is in a Bell state and can be expressed as

$${|\psi \rangle }_{\mathrm{in}}=\frac{1}{\sqrt{2}}\left({|\ell ,p\rangle }_{\mathrm{A}}{|-\ell ,p\rangle }_{\mathrm{B}}+{|-\ell ,p\rangle }_{\mathrm{A}}{|\ell ,p\rangle }_{\mathrm{B}}\right),$$

(1)

where the footnotes A and B represent two different paths of photons, $p$ is the radial quantum number, and $\ell$ is the azimuthal mode order of the Laguerre-Gaussian (LG) beam. In the cylindrical coordinates, a single photon LG mode can be expressed as [22].

$$\langle r|\ell \rangle =\frac{1}{\sqrt{2\pi }}{R}_{\ell ,p}(r,z)\exp (i\ell \theta ),$$

(2)

where $r^2=x^2+y^2$, and the parameter $\theta$ is the azimuthal angle. The LG function $R_{\ell ,p}(r,z)$ in normalized cylindrical coordinates can be written as [26,27,28]

$$R_{\ell ,p}(r,z)=\frac{A_{lp}}{w\left(\mathrm{z}\right)}{\left(\frac{\sqrt{2}r}{w\left(\mathrm{z}\right)}\right)}^{|\ell |}{L}_p^{|\ell |}\left(\frac{2r^2}{w^2\left(\mathrm{z}\right)}\right)\exp \left(-\frac{r^2}{w^2\left(\mathrm{z}\right)}\right)\exp \left\{\mathrm{i}(\ell +1){\tan }^{-1}(z/z_R)-\frac{\mathrm{i}k{r}^2}{2z\left[1+{(z_R/z)}^2\right]}\right\},$$

(3)

Here $A_{\ell p}={\left(\frac{p!2^{|\ell |}}{\pi (p+|\ell |)!}\right)}^{1/2}$ is a normalization constant, the parameter $w=w_0\sqrt{1+(\mathrm{z}/{\mathrm{z}}_R{)}^2}$ is related to the propagation distance $z$ and initial beam radius $w_0$, and the Rayleigh range ${\mathrm{z}}_R=k{w}_0^2/2$ is the waist radius of the Gaussian beam in the receiver plane. The Rayleigh range is correlated with the wavelength $\lambda$ by the ratio $k=2\pi /\lambda$ (the wave number), and $L_p^{|\ell |}(\cdot )$ represents the associated Laguerre polynomials.

As the photons travel through the turbulent atmosphere, OAM modes are distorted by the modulations of the random phase of the turbulent atmosphere, leading to the decay of OAM entanglement. Generally, the output density matrix ${\rho }_{\mathrm{out}}$ is used for determining the OAM entanglement after passing through turbulence [14,17,24], and

$${\rho }_{\mathrm{out}}={\displaystyle {\sum }_{mn{m}^{\prime }{n}^{\prime }}{\rho }_{m,n,m^{\prime },n^{\prime }}{|{\ell }_m,{\ell }_{m^{\prime }}\rangle }_{\mathrm{AB}}}\langle {\ell }_{n^{\prime }},{\ell }_n|.$$

(4)

${\rho }_{m,n,m^{\prime },n^{\prime }}$ is the density matrix element of output state [17,24], and

$${\rho }_{m,n,m^{\prime },n^{\prime }}=\langle {\ell }_{m^{\prime }},{\ell }_m|{\psi }_I\rangle \langle {\psi }_I|{\ell }_n,{\ell }_{n^{\prime }}\rangle ,$$

(5)

where $|{\ell }_m\rangle$($|{\ell }_{m^{\prime }}\rangle$) and $|{\ell }_{\mathrm{n}}\rangle$($|{\ell }_{n^{\prime }}\rangle$) are direct measurement states. The input state ${|\psi \rangle }_{in}$ propagating through the atmospheric turbulence changes into the state $|{\psi }_I\rangle$. In the weak turbulence regime, the impacts of the turbulent atmosphere on OAM photons are equivalent to phase errors in the transverse beam profile [22], leading to

$$\langle r|{\psi }_I\rangle ={\frac{1}{\sqrt{2}}}^{(\langle r{|\ell \rangle }_{\mathrm{A}}\langle r{|-\ell \rangle }_{\mathrm{B}}{\mathrm{e}}^{\mathrm{i}\left({\varphi }_A\left(r\right)+{\varphi }_B\left(r\right)\right)}+\langle r{|-\ell \rangle }_{\mathrm{A}}\langle r{|\ell \rangle }_{\mathrm{B}}{\mathrm{e}}^{\mathrm{i}\left({{\varphi }^{\prime }}_A\left(r\right)+{{\varphi }^{\prime }}_B\left(r\right)\right)})},$$

(6)

where the random perturbations ${\varphi }_j\left(r\right)$ and ${{\varphi }^{\prime }}_j\left(r\right)$ ($j=\mathrm{A},\mathrm{B}$) are induced by two weakly turbulent atmospheres.

Note that the scintillation process can make the OAM modes spread through the entire Hilbert space. To deal with an infinite-dimensional Hilbert space of output states upon detection, the truncated Hilbert space is necessary. In this paper, at first we extract the OAM information contained in the modes, which are $\pm \ell \pm 1$ and $\pm \ell$, and then project the transmitted state on encoding subspace $|\ell ,\ell \rangle ,|\ell ,-\ell \rangle ,|-\ell ,\ell \rangle ,|-\ell ,-\ell \rangle$. Hilbert-space truncation does keep track of the scattering to density matrix elements that are inside the subspace, but the backward scattering from outside the subspace to elements in the encoding subspace is lost. Because OAM modes that are outside the subspace can also be scattered back to the encoding subspace due to scintillation, the backward scattering is very important for evaluating the evolution of OAM entanglement through turbulence. Considering the effect of backward scattering, the output density matrix ${\rho }_{\mathrm{out}}$ is readily found to be [24]

$$\left(\begin{array}{cccc}{\rho }_{11}& 0& 0& 0\\ 0& {\rho }_{22}& {\rho }_{23}& 0\\ 0& {\rho }_{32}& {\rho }_{33}& 0\\ 0& 0& 0& {\rho }_{44}\end{array}\right).$$

(7)

For $|\ell |=1$, the matrix elements are described by

$${\rho }_{11}=4ab{c}_1{c}_2+2ab,$$

(8)

$${\rho }_{22}=c_1^2{c}_2^2+2a^2{c}_1{c}_2+2b^2{c}_1{c}_2+a^2+b^2,$$

(9)

$${\rho }_{23}=c_1^2{c}_2^2+2a^2{c}_1{c}_2+a^2,$$

(10)

$${\rho }_{32}={\rho }_{23},$$

(11)

$${\rho }_{33}={\rho }_{22},$$

(12)

$${\rho }_{44}={\rho }_{11}.$$

(13)

Otherwise

$${\rho }_{11}=2ab\left(2c_1{c}_2+2c_1{c}_3+1\right),$$

(14)

$${\rho }_{22}=c_1^2{\left(c_2+c_3\right)}^2+\left(a^2+b^2\right)\left(2c_1{c}_3+2c_1{c}_2+1\right),$$

(15)

$${\rho }_{33}=2c_1^2{c}_3\left(c_2+c_3\right)+\left(a^2+b^2\right)\left(3c_1{c}_3+c_1{c}_2+1\right),$$

(16)

$${\rho }_{44}=2ab\left(c_1{c}_2+3c_1{c}_3+1\right),$$

(17)

$${\rho }_{23}=c_1^2{\left(c_2+c_3\right)}^2+a^2\left(2c_1{c}_3+2c_1{c}_2\right)+a^2,$$

(18)

$${\rho }_{32}=c_1^2{\left(c_2+c_3\right)}^2+a^2\left(2c_1{c}_3+2c_1{c}_2\right)+a^2,$$

(19)

where $a$ is the survival amplitude with $\left|\Delta \ell \right|=0$ [14], $b$ is crosstalk amplitude with $\left|\Delta \ell \right|=2\ell$ [14], and $c_j(j=1,2,3)$ is also crosstalk amplitude but $\left|\Delta \ell \right|=1$ [24],

$$a={\left|\langle {\psi }_{\pm \ell }|\pm \ell \rangle \right|}^2=\frac{1}{2\pi }{{\displaystyle {\int }_0^{\infty }r\left|R_{\ell ,p}(r)\right|}}^2\mathrm{d}r{\displaystyle {\int }_0^{2\pi }\mathrm{d}}\theta \exp [-0.5D_{\varphi }\left(2r\left|\sin (\theta /2)\right|\right)],$$

(20)

$$b={\left|\langle {\psi }_{\pm \ell }|\mp \ell \rangle \right|}^2=\frac{1}{2\pi }{{\displaystyle {\int }_0^{\infty }r\left|R_{\ell ,p}(r)\right|}}^2\mathrm{d}r{\displaystyle {\int }_0^{2\pi }\mathrm{d}}\theta \exp (-2\mathrm{i}\ell \theta )\exp [-0.5D_{\varphi }\left(2r\left|\sin (\theta /2)\right|\right)],$$

(21)

$$c_1={\left|\langle {\psi }_{\pm \ell }|\pm \ell \pm 1\rangle \right|}^2=\frac{1}{2\pi }{{\displaystyle {\int }_0^{\infty }r\left|R_{\ell ,p}(r)\right|}}^2\mathrm{d}r{\displaystyle {\int }_0^{2\pi }\mathrm{d}}\theta \exp (-\mathrm{i}\theta )\exp [-0.5D_{\varphi }\left(2r\left|\sin (\theta /2)\right|\right)],$$

(22)

$$c_2={\left|\langle {\psi }_{\pm \ell \pm 1}|\pm \ell \rangle \right|}^2=\frac{1}{2\pi }{{\displaystyle {\int }_0^{\infty }r\left|R_{\pm \ell \pm 1,p}(r)\right|}}^2\mathrm{d}r{\displaystyle {\int }_0^{2\pi }\mathrm{d}}\theta \exp (-\mathrm{i}\theta )\exp [-0.5D_{\varphi }\left(2r\left|\sin (\theta /2)\right|\right)],$$

(23)

$$c_3={\left|\langle {\psi }_{\pm \ell \mp 1}|\pm \ell \rangle \right|}^2=\frac{1}{2\pi }{{\displaystyle {\int }_0^{\infty }r\left|R_{\pm \ell \mp 1,p}(r)\right|}}^2\mathrm{d}r{\displaystyle {\int }_0^{2\pi }\mathrm{d}}\theta \exp (-\mathrm{i}\theta )\exp [-0.5D_{\varphi }\left(2r\left|\sin (\theta /2)\right|\right)].$$

(24)

Here we use the non-Kolmogorov power spectrum for the investigation of the evolution of OAM entanglement in turbulence. The non-Kolmogorov power spectrum for the refractive index fluctuations is given by [29,30]

$${\Phi }_n(\kappa ,\alpha )=A(\alpha ){\tilde{C}}_n^2{({\kappa }^2+{\kappa }_0^2)}^{-\alpha /2}\exp (-{\kappa }^2/{\kappa }_m^2),\begin{array}{cc}& \end{array}3<\alpha <4,$$

(25)

$\alpha$ being the generalized exponent, ${\tilde{C}}_n^2$ (in units of ${\mathrm{m}}^{\alpha -3}$) being a generalized refractive-index structure parameter, ${\kappa }_0=2\pi /L_0$, $L_0$ representing the outer scale of turbulence, ${\kappa }_m=c\left(\alpha \right)/l_0$, $l_0$ representing the inner scale of turbulence, and $\kappa$ being the magnitude of the three-dimensional wave number vector, and

$$c\left(\alpha \right)={\left(\Gamma (5-\alpha /2)A(\alpha )2\pi /3\right)}^{\frac{1}{\alpha -5}},$$

(26)

$$A(\alpha )=1/4{\pi }^2\Gamma (\alpha -1)\cos \left(\alpha \pi /2\right),$$

(27)

where $\Gamma (x)$ is the gamma function of the term. When $\alpha =11/3$, $L_0=\infty$, $l_0=0$, and ${\tilde{C}}_n^2=C_n^2$, Equation (25) can be reduced to the conventional Kolmogorov spectrum [29]

$${\mathrm{\Phi }}_n(\kappa )=0.033C_n^2{\kappa }^{-11/3}.$$

(28)

$D_{\varphi }\left(r\right)$ is a two-point spherical wave structure function that contains the influence of atmospheric turbulence, which can be expressed as [31,32]

$$D_{\varphi }\left(r_1,r_2;z\right)=8{\pi }^2{k}^{2}z{\displaystyle {\int }_0^1\mathrm{d}}\varsigma {\displaystyle {\int }_0^{\infty }\left\{1-J_0\left[\kappa \left|\varsigma \left(r_1-r_2\right)\right|\right]\right\}{\mathrm{\Phi }}_n(\kappa ,\alpha )}\kappa \mathrm{d}\kappa ,$$

(29)

where $\varsigma$ denotes the normalized distance variable, $J_0(\cdot )$ is the zero-order Bessel function of the first kind and has the approximation

$$J_0\left(\kappa \left|\varsigma \left(r_1-r_2\right)\right|\right)=1-\frac{1}{4}{\left(\kappa \left|\varsigma \left(r_1-r_2\right)\right|\right)}^2.$$

(30)

Under the quadratic approximation of Rytov’s phase structure function [32,33,34,35], the term $\exp [-0.5D_{\varphi }\left(2r\left|\sin (\theta /2)\right|\right)]$ can be written as

$$\exp [-0.5D_{\varphi }\left(2r\left|\sin (\theta /2)\right|\right)]=\exp \left[-{\left({2r\left|\sin \left(\theta /2\right)\right|/\rho }_0\right)}^2\right],$$

(31)

where ${\rho }_0$ is the spatial coherence length of a spherical wave propagating in a non-Kolmogorov turbulent atmosphere, and [32]

$${\rho }_0={\left(\frac{{\pi }^2{k}^{2}zA\left(\alpha \right)}{6\left(\alpha -2\right)}{\tilde{C}}_n^2[{\kappa }_m^{2-\alpha }\exp (\frac{{\kappa }_0^2}{{\kappa }_m^2})\left(2{\kappa }_0^2-2{\kappa }_m^2+\alpha {\kappa }_m^2\right)\Gamma (2-\frac{\alpha }{2},\frac{{\kappa }_0^2}{{\kappa }_m^2})-2{\kappa }_0^{4-\alpha }]\right)}^{-1/2}.$$

(32)

The propagation of the states $|\ell \rangle$($|-\ell \rangle$) and $|\pm \ell \pm 1\rangle$($|\pm \ell \mp 1\rangle$) through atmospheric turbulence change into the states $|{\psi }_{\ell }\rangle$($|{\psi }_{-\ell }\rangle$) and $|{\psi }_{\pm \ell \pm 1}\rangle$($|{\psi }_{\pm \ell \mp 1}\rangle$), respectively.

Wootter’s concurrence is used to evaluate the entanglement degree of the output bipartite OAM state [25], which is given by

$$C\left(\rho \right)=\max \left\{0,{\lambda }_1-{\lambda }_2-{\lambda }_3-{\lambda }_4\right\},$$

(33)

where ${\lambda }_i$ are the eigenvalues of the Hermitian matrix $\xi$, which are ranked by decreasing order, and

$$\xi ={\rho }_{\mathrm{out}}({\sigma }_y\otimes {\sigma }_y){\rho }_{\mathrm{out}}^{\ast }({\sigma }_y\otimes {\sigma }_y),$$

(34)

Asterisk (*) indicating the conjugate of a complex number, ${\sigma }_y$ given by

$${\sigma }_y=\left(\begin{array}{cc}0& -\mathrm{i}\\ \mathrm{i}& 0\end{array}\right).$$

(35)

3. Numerical Results and Analysis

Firstly, our results of numerical evaluation are compared with the results based on S&R theory [9]. The turbulence parameters are set to be $\alpha =11/3,$ $L_0=500 \mathrm{m},$ and $l_0=1 \mathrm{mm}$. As shown in Figure 2, the results of numerical evaluation agree with S&R theory well when $|\ell |\le 3$ and $p=0$. In other cases, the results of numerical evaluation deviate significantly from the result in S&R theory. Consequently, the effect of backward scattering can be ignored when OAM is in lower-order mode, but it is very crucial for higher-order OAM entanglement.

Now the entanglement evolution of the higher-order OAM entangled state in non-Kolmogorov weak turbulence is investigated. In the following numerical examples, the beam parameters are set to be $\ell =3$, $p=2$, $w_0=0.08 \mathrm{m}$, and $\lambda =1064 \mathrm{nm}$, and the parameters of turbulence are set to be $\alpha =3.6$, $L_0=10 \mathrm{m},$ $l_0=1\mathrm{mm},$ and ${\tilde{C}}_n^2=8\times {10}^{-14}{\mathrm{m}}^{3-\alpha }$, unless otherwise specified. The results of the numerical evaluation are presented in Figure 3, Figure 4, Figure 5 and Figure 6.

Figure 3 shows the concurrence versus the propagation distance $\mathrm{z}$ for different beam parameters. As shown in Figure 3a,b, the concurrence lasts longer for higher value of the azimuthal mode and larger radial quantum number. Moreover, one observes that when the entangled photon propagates only a relatively short distance within 100 m, the concurrence decays quickly for larger radial quantum number, shown in Figure 3a. Such results can be interpreted as follows. As shown in Figure 4, the density matrices for a pair of entangled qutrits are $4\times 4$ matrices. For z =0 m, the magnitudes of the central density elements are all 0.5, and the input states have the highest purity. The same heights (magnitudes of the elements) indicate that the input state is maximally entangled [21]. For z = 50 m, the central elements in the density matrix vary more significantly as the value of radial quantum number increases, meaning that the purity decreases quickly for OAM entanglement with the radial quantum number increasing. When the propagation distance is 300 m, the diagonal elements in the density matrix grow more rapidly at the cost of the central density elements that represent the original input state [21]. However, the diagonal elements dominate over the other elements more slowly as the value of the radial quantum number increases, meaning that OAM entanglement with higher radial quantum number is more robust. These results also reflect the fact that scattering from one OAM state to another depends not only on the change in OAM ($\Delta \ell$) [9], but also on different radial intensity profiles $R_{\ell ,p}(r,z)$.

Figure 5 presents the dependence of the concurrence on turbulence parameters for different propagation distances. From Figure 5a, it can be seen that as the generalized exponent increases, the concurrence drops off sharply to a minimum value at about 3.07, and then gradually increases to the maximum value. In addition, when $\alpha$ reaches around 3.07, OAM entanglement gradually decreases to zero for $\mathrm{z}\ge 100 \mathrm{m}$. Such a phenomenon suggests that the condition of turbulence with the generalized exponent around $\alpha =3.07$ is not suitable for OAM entanglement transmission. This can be understood as follows: as shown in Figure 6, the spatial coherence length ${\rho }_0$ first decreases as $\alpha$ increases, reaches a minimum value when $\alpha$ is about 3.07, and then increases with further increase of $\alpha$. The LG beam suffers the most serious perturbation when $\alpha$ is about 3.07 [28]. As a result, the influence of turbulence on the OAM entanglement is the most serious near $\alpha =3.07$. Figure 5b demonstrates the fact that the OAM entanglement always decays in the weak turbulence, but the rate of decay becomes very slow when the value of the refractive-index structure parameter decreases. That is, the entanglement evolution of the OAM state will be impacted less by turbulence with a smaller refractive-index structure parameter. Figure 5c denotes that the concurrence lasts longer for a smaller value of the turbulence outer scale, revealing that the entanglement evolution of the OAM state will be impacted more severely by turbulence with a larger outer scale. It can also be seen that under the condition $L_0\ge 1\mathrm{m}$, the influence of outer scale on the entanglement evolution of the OAM state is very slight. In Figure 5d, it can be found that the concurrence can survive over a longer distance with increasing turbulence inner scale. This means that turbulence with a lager inner scale has less influence on the OAM entanglement.

4. Discussion and Conclusions

In this paper, the entanglement evolution of OAM photons with higher-order OAM mode propagating across a non-Kolmogorov turbulent atmosphere has been numerically evaluated. Here, we only considered the case that two photons both have passed through turbulence. The expression for the output density matrix of entangled photons with higher-order OAM mode has been obtained. In contrast with the result based on S&R theory, the output density matrix takes into account the effect of backward scattering. The results of numerical evaluation show that the effect of backward scattering can be ignored for OAM entanglement in lower-order mode, while it is very crucial for higher-order mode OAM entanglement.

Quadratic approximation of the non-Kolmogorov phase structure function is used to estimate the evolution of OAM entanglement. When the non-Kolmogorov power spectrum is reduced to the Kolmogorov spectrum and the effect of backward scattering can be ignored, our numerical results are consistent with the results reported by Bachmann et al [36], who analyzed the universal entanglement decay laws for the quadratic approximation.

There are various aspects that pose challenges to experimental work on the propagation of entangled photons with higher-order OAM mode entangled states through turbulence. In practical scenarios it is more difficult and complex to produce entangled photon pairs with larger radial quantum number. In addition, it is also observed that modes with higher value of the azimuthal mode are more difficult to measure experimentally. Therefore, more work remains to be done in the future.

In summary, the decay of entangled orbital angular momentum (OAM) photons propagating across non-Kolmogorov turbulence has been investigated. In this work, we explore the evolution of OAM entanglement in the weak scintillation regime and consider the effect of backward scattering on OAM entanglement with higher-order OAM mode. The results of the numerical evaluation reveal that the concurrence monotonically decreases in turbulence, but the OAM entangled state with higher value of the azimuthal mode and larger radial quantum number lasts much longer, which means OAM entangled states with higher value of the azimuthal mode and larger radial quantum number are more appropriate to quantum communication over long distances. Meanwhile, non-Kolmogorov turbulence with a smaller refractive-index structure parameter, a smaller turbulence outer scale or a larger turbulence inner scale affects OAM entanglement evolution less. In addition, the influence of turbulence on the entanglement evolution of the OAM state is the most serious when the generalized exponent is around 3.07, and thus the condition of turbulence with the generalized exponent around 3.07 is not suitable for OAM entanglement transmission. Our findings will be very important to improve the performance of a free-space quantum communication system.