Shuqin Lin, Yangjian Cai, Jiayi Yu. Research progress of propagation of beams with special correlation structure in turbulent atmosphere[J]. High Power Laser and Particle Beams, 2021, 33(8): 081006
- High Power Laser and Particle Beams
- Vol. 33, Issue 8, 081006 (2021)
![Evolution of the spectral density of the multi-Gaussian Schell-model beams propagating in turbulent atmosphere (solid curve N=1，dashed curve N=4，dotted curve N=10，and dash-dotted curve N=40)[82]](/richHtml/qjglzs/2021/33/8/081006/img_1.jpg)
Fig. 1. Evolution of the spectral density of the multi-Gaussian Schell-model beams propagating in turbulent atmosphere (solid curve N =1，dashed curve N =4，dotted curve N =10，and dash-dotted curve N =40)[82]
![Normalized propagation factor of multi-Gaussian Schell-model beams propagating in turbulent atmosphere[37]](/richHtml/qjglzs/2021/33/8/081006/img_2.jpg)
Fig. 2. Normalized propagation factor of multi-Gaussian Schell-model beams propagating in turbulent atmosphere[37]
![3D-normalized spectral intensity distribution (a) and S(0,z)/Smax(ρ,z) ratio of the spectral intensity (b) of Hermite-Gaussian correlated Schell-model beams on propagation in turbulent atmosphere[48]](/Images/icon/loading.gif){kind=icon}
Fig. 3. 3D-normalized spectral intensity distribution (a) and S(0,z )/Smax(ρ ,z ) ratio of the spectral intensity (b) of Hermite-Gaussian correlated Schell-model beams on propagation in turbulent atmosphere[48]
Fig. 4. Normalized propagation factors of Hermite-Gaussian correlated Schell-model beams in x direction (a) and y direction (b) in turbulent atmosphere[48]
Fig. 5. Beam wander of Hermite-Gaussian correlated Schell-model beams in turbulent atmosphere in theory and experiment[61]
Fig. 6. Evolution of the spectral density of the non-uniformly correlated beams in free space[95]
Fig. 7. Evolution of the (a) scintillation and (b) spectral density of non-uniformly correlated beams in turbulent atmosphere[96]
Fig. 8. Evolution of the spectral density of the Hermite non-uniformly correlated beams in turbulent atmosphere[59]
Fig. 9. Normalized intensity on-axis (a)～(c) and scintillation on-axis (d)～(f) of Hermite non-uniformly correlated beams in turbulent atmosphere[59]
Fig. 10. Evolution of spectral intensity of Hermite non-uniformly correlated array beams with (a) m = 1，p = q = 1，r c= 3 cm，x 0= y 0= 3 cm；(b) m = 1，p = q = 1，r c= 3 cm，x 0= y 0= 5 cm；(c) m = 2，p = q = 1，r c= 3 cm，x 0= y 0= 5 cm；(d) m = 2，p =q = 2，r c= 3 cm，x 0= y 0= 5 cm；(e) m = 2，p = q = 2，r c= 5 cm，x 0= y 0= 5 cm in turbulent atmosphere[67]
Fig. 11. Evolution of ratio intensity and degree of polarization of radially polarized Hermite non-uniform correlation beams in free space[98]
Fig. 12. Evolution of spectral intensity of (a) conventional radially polarized partially coherent beams and radially polarized Hermite non-uniform correlation beams with different mode orders (b) m =0 (c) m =1 in turbulent atmosphere[66]
Fig. 13. Ratio of the spectral intensity of radially polarized Hermite non-uniform correlation beam in turbulence atmosphere[66]
Fig. 14. Percentage of intensity of the completely polarized portion of radially polarized Hermite non-uniform correlation beam in turbulence atmosphere[66]
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