## 1 Introduction  
Fluctuations in the refractive index of the atmosphere, also known as optical turbulence, are caused by the wind blowing over the earth's surface and the temperature gradient between the earth's surface and the above air [1]. Atmospheric turbulence is a primary reason for laser beam wandering and spreading. It affects the observation of astronomical telescopes by limiting imaging quality and interfering with the propagation of laser beams [2, 3]. Atmospheric turbulence strength is generally characterized by the structural parameters of the refractive index \(\left(C_{n}^{2}\right)\). Appropriate knowledge of \(C_{n}^{2}\) and further understanding of optical turbulence characteristics are essential for improving the performance of adaptive optics (AO) systems and conducting astronomical observations. Since the 1960s, quantitative measurement of optical turbulence strength of the visible light range at different heights is required in modern astronomy to improve the visibility of the focus of existing telescopes and to find new locations where new instruments can be installed [4]. Astronomical site selection is a long and arduous process that requires a lot of manpower, material resources and financial resources. In order to deploy powerful facilities for astronomical observations, it is necessary to carry out many atmospheric optical turbulence investigations on astronomical locations. Investigating the optical turbulence over the ocean helps to further understand the atmosphere of the environment. Previously, some studies have been conducted on the ocean atmosphere. The structures and characteristics of a windy atmospheric boundary layer during a cold air outbreak in the ocean region are investigated by [PERSON], who found that the main structures and characteristics are the same as during strong wind episodes with cold air outbreaks on land [5]. Based on data from the board measurement test through South China Sea Monsoon Experiment-II during June 2019, for the first time, the spatiotemporal distribution of optical turbulence over the South China sea and its sea surface was analyzed comprehensively by [PERSON] et al. [6]. However, this study lacks the measured optical turbulence profile data. Additionally, [PERSON] analyzed the Tropical Rainfall Measuring Mission Microwave Imager data for the period 1998-2007, which reveals large subseasonal fluctuations in sea surface temperature during the summer monsoon onset [7]. A study that analyzed radiosonde data was performed by [PERSON] at various different astronomical sites. This was the first time that a complete median and average \(C_{n}^{2}\) and outer scale profile, from the ground up to 30 km, was available [8]. The WRF Model was used to forecast the routine meteorological parameters firstly, and then was calculated based on these parameters by the Bulk model from the Monin-Obukhov similarity theory over the ocean near-surface, which was introduced by [PERSON] and [PERSON] [9]. Using the data from Shack-Hartmann wavefront sensor and reanalysis data, [PERSON] et al. presented the first seasonal study of the vertical distribution of wind speed and daytime optical turbulence conditions at the Baikal Astrophysical Observatory [10]. Furthermore, [PERSON] and [PERSON] offered an investigation relevant to latent heat flux exchanges at the air-sea interface, which play important roles in the formation and development of tropical cyclones over the ocean [11]. [PERSON] and [PERSON] presented an analysis of the first boundary layer flight observations on the ocean by the Hong Kong Observatory comprising four eyewall penetrations, which derived the vertical flux of momentum and vertical momentum diffusivity from observed turbulence parameters [12]. Based on generalizations of numerous measurements and calculations, [PERSON] found that the outer scale of turbulence in the surface layer of the atmosphere depends not only on the height above the underlying surface but also on the type of atmospheric stratification [13].