## 2 Materials and Methods
### Geographic Polarization Suppression Model  
#### 2.2.1 Real-Time Positioning Information Solution Method  
Based on the analysis of the three-dimensional schematic of light reflection on the sea surface, the geometric relationship between the angle of incidence and the solar or lunar altitude angle is determined. As shown in Figure 2, S represents the position of the  
Figure 1: General methodological flowchart for sea surface glare suppression. sun or moon, O is the point of reflection on the sea surface, and P is the camera position, with \(A_{s}\) representing the solar or lunar azimuth angle, \(h_{s}\) the solar or lunar altitude angle, and \(\theta\) the angle of incidence of the solar or lunar light on the sea surface. The geometric relationship between the angle of incidence and the solar or lunar altitude angle, as derived from Figure 2, is as follows:  
\[\theta=90^{\circ}-h_{s} \tag{3}\]  
The solar and lunar altitude angles \(h_{s}\) are calculated based on real-time information, and the calculation method is as follows. Solar Position Calculation  
\[\cos A_{s}=\frac{\sin\delta-\sinh_{s}\sin\varphi}{\cosh_{s}\cos\varphi} \tag{4}\]  
\[\sinh_{s}=\sin\varphi\sin\delta+\cos\varphi\cos\delta\cos t \tag{5}\]  
In the equation, \(\delta\) represents the solar declination angle; \(\varphi\) is the observer's latitude; \(t\) is the solar hour angle; \(h_{s}\) is the solar altitude angle; and \(A_{s}\) is the solar azimuth angle. The solar declination angle is calculated using the Yu operator, and the solar hour angle \(t\) is calculated using the Wloof operator [19]. The lunar longitude and latitude are calculated using the lunar calculation scheme referenced in ELP/MPP02 [20] and the lunar position periodic term calculation table developed from document [21], as shown in Equation (6). \[\left\{ \begin{array}{l}\lambda_{m}=V+L_{0}+L_{1}T+L_{2}T^{2}\\ \beta_{m}=B_{0}+B_{1}T\end{array} \right. \tag{6}\]  
Here, \(\lambda_{m}\) represents the lunar longitude; \(\beta_{m}\) represents the lunar latitude; \(V\) is the mean lunar longitude; \(L_{0},L_{1},L_{2}\) is the longitude perturbation term; \(B_{0},B_{1}\) is the latitude perturbation term; and \(T\) represents the number of relative Julian centuries. The perturbations in longitude and latitude can be calculated using the periodic term calculation table from document [21]. Subsequently, the longitude and latitude are converted into right ascension and declination, as shown in Equation (7):  
\[ \begin{array}{l}\tan\alpha_{m}=\frac{\sin\lambda_{m}\cos\varepsilon_{m}-\tan \beta_{m}\sin\varepsilon_{m}}{\cos\lambda_{m}}\\ \sin\delta_{m}=\sin\beta_{m}\cos\varepsilon_{m}+\cos\beta_{m}\sin\varepsilon_ {m}\sin\lambda_{m}\end{array}  \tag{7}\]  
Figure 2: Three-dimensional schematic of the sun and moon reflections on the sea surface. Here, \(\alpha_{m}\) represents the right ascension, \(\delta_{m}\) represents the lunar declination, and \(\varepsilon_{m}\) represents the obliquity of the ecliptic. The formula for calculating the obliquity of the ecliptic is shown as Equation (8):  
\[\varepsilon_{m}=23.4392911111-\frac{46.815}{3600}T-\frac{0.00059}{3600}T^{2}+ \frac{0.001813}{3600}T^{3} \tag{8}\]  
The lunar hour angle is calculated using the lunar right ascension \(\alpha_{m}\), and the calculation is as follows:  
\[t_{m}=Q+\sigma-\alpha_{m} \tag{9}\]  
Here, \(t\) represents the lunar hour angle, \(Q\) represents Greenwich sidereal time, and \(\sigma\) represents the longitude value of the observation point. Finally, the lunar declination and lunar hour angle are converted into the lunar azimuth angle and altitude angle. \[ \begin{array}{l}\tan A_{m}=\frac{\sin t_{m}}{\cos t_{m}\sin\varphi-\tan \delta_{m}\cos\varphi}\\ \sinh_{m}=\sin\varphi\sin\delta_{m}+\cos\varphi\cos\delta_{m}\cos t_{m}\end{array}  \tag{10}\]  
Here, \(A_{m}\) represents the lunar azimuth angle, \(h_{m}\) represents the lunar altitude angle, and \(\varphi\) represents the latitude value of the observation point.