Research progress on numerical simulations of long space laser propagation

Hua Zheyi; Xu Zhaorui; Peng Shaojing; Liu Ye; Liu Chong; Wu Lan; Liu Dong

doi:10.12086/oee.2024.230185

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Hua Z Y, Xu Z R, Peng S J, et al. Research progress on numerical simulations of long space laser propagation[J]. Opto-Electron Eng, 2024, 51(2): 230185. doi: 10.12086/oee.2024.230185

Citation:

Hua Z Y, Xu Z R, Peng S J, et al. Research progress on numerical simulations of long space laser propagation[J]. Opto-Electron Eng, 2024, 51(2): 230185. doi: 10.12086/oee.2024.230185

Research progress on numerical simulations of long space laser propagation

State Key Laboratory of Modern Optical Instrumentation, College of Optical Science and Engineering, Zhejiang University, Hangzhou, Zhejiang 310027, China

Fund Project: Project supported by National Key Research and Development Program of China (2021YFC2202001)

More Information

Corresponding author: liudongopt@zju.edu.cn

Received Date 26 July 2023

Revised Date 17 November 2023

Accepted Date 23 November 2023

Available Online 29 March 2024

Published Date 29 February 2024

Abstract

Abstract

This paper mainly introduces the development of space gravitational wave transmission and laser propagation in space gravitational wave detection. We profile the calculation methods used in the simulation of laser propagation and jitter noise in space-based laser interferometry. Compared with ground detection, space gravitational wave detection can effectively reduce noise and increase the length of the interference arm to realize high-precision gravitational wave detection. Under the distance of millions of kilometers and the precision requirements of the picometer level, it is necessary to consider the phase noise caused by pointing jitter with the telescope. Research has shown that defocus and astigmatism are the main aberrations affecting jitter noise at a distance of 2.5×10⁹m. There is a deviation between the phase stationary point and the origin position. To minimize the phase noise, the telescope angle needs to be adjusted. The gravitational wave detection at the phase stationary point can effectively reduce the phase noise and the requirements of the telescope exit pupil wavefront RMS. The large defocus and small coma can make the phase stationary point close to the optical axis and increase the received laser power.
- gravitational wave detection /
- space propagation /
- jitter noise /
- phase stationary point

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References

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Overview

Overview

Compared with ground gravitational wave detection, space gravitational wave detection can avoid the low-frequency noise caused by ground vibration and the interference of climate change on the transmission. The space environment can also greatly increase the arm length of laser interference to achieve high-precision gravitational wave detection. However, the ultra-long inter-satellite link transmission distance also puts forward extremely high requirements for pointing accuracy and dynamic measurement capabilities. At a transmission distance of millions of kilometers, the detection accuracy needs to reach the picometer level.

To minimize the influence of noises on the detection, we must simulate the system with high precision. The simulation of inter-satellite transmission can be realized by Hermite Gaussian beam fitting, Fourier transform or numerical integration. The plasma has little effect on inter-satellite transmission under most circumstances. It will thus not affect the detection. Pointing jitter noise is the focus of research in inter-satellite transmission. In the actual system, there are aberrations in the exit pupil wavefront of the telescope, so the far-field wavefront is no longer close to the ideal spherical wave. An angle offset of 10 nrad will cause a position offset of tens of meters in the far field. In the analysis, the far-field origin is usually taken as the object, and the phase part of the telescope exit pupil complex amplitude is expanded to simplify the model in a Taylor series. The coupling coefficients between the far field and the exit pupil Zernike aberration of the telescope can be calculated by the integral calculation or the least square fitting. To satisfy the simulation accuracy of the picometer level, the Taylor expansion and the coupling coefficients should retain at least the second-order term.

Taking the LISA system as a reference, the phase noise of the inter-satellite transmission needs to be less than 1 pm. Research has shown that the defocus and the astigmatism are the main aberrations affecting jitter noise at a distance of 2.5×10⁹m. There is a deviation between the phase stationary point and the origin position. To minimize the phase noise, the telescope angle needs to be adjusted. The gravitational wave detection at the phase stationary point can effectively reduce the phase noise and the requirements of the telescope exit pupil wavefront RMS. The large defocus and small coma can make the phase stationary point close to the optical axis and increase the received laser power.