# Enhancing Meteor Observations with Photodiode Detectors
## 5 Discussion  
In Figures 8 and 9, a substantial brightness difference is apparent between the brightest and faintest detections, reaching a factor of 50 or more. The brightest meteors show a peak amplitude that is several hundreds times greater than the noise level, indicating significant dynamics of the phenomena observed the proposed way. The shapes of the waveforms  
Figure 10: Sample six meteor detections registered by ASI ZWO178 MM camera (exposure time 60 s, timing given in each figure, compare with Figure 8 and Figure 9). Figure 9: Examples of meteor detections registered by our photodiode detector on the second day of Perseids maximum, 12 August 2023.  
vary; some increase slowly, reaching a maximum, then decrease rapidly, while others are symmetrical around the peak or present even the opposite character. Although analyzing the origins of these waveform shapes is beyond the scope of this discussion, it will be a focus of future research. In the upcoming years of operation with our instrument in a remote observatory and a sufficient number of recordings, more accurate analyzes will be possible. Figure 10A exposes the brightest meteor that was recorded during the two days of observation. Pixel saturation is evident in this image, making it impossible to accurately analyze the brightness of the object from the photograph. The phenomenon, despite its brief presence in the sky of less than half a second, is bright enough that even with a faster camera and shorter exposure time, the result would be similar. Pixel saturation is a significant problem because it prevents precise photometric analysis. On the other hand, the results obtained with our photodiode detector are free of saturation proving the dynamic range inaccessible for recordings with image sensors. Figure 10B presents a meteor with a much lower brightness compared to example A. Interestingly, at least two other streaks of light are present in the same image, resulting from the passage of satellites. The similar brightness levels of these objects can pose a challenge in the automatic identification of meteors, highlighting the importance of image sequence analysis. In our case, visual analysis of the before-and-after images allowed us to distinguish between meteors and satellites, which is an added value in the context of meteor identification. Figure 10C shows a phenomenon that is likely the result of fragmentation of the meteor during its passage through the atmosphere. The image reveals a terminal flare, consistent with the anomalous brightness pattern recorded by our detector, featuring a long rise time followed by a short, sharp pulse. Such analysis may allow us to identify and understand the complex phenomena associated with meteor fragmentation. Figure 10D shows a meteor low above the horizon whose image is significantly blurred by the atmosphere. Despite this, our detector, aimed at the zenith, was able to detect this phenomenon. This observation demonstrates the ability of our detector to record meteors even under difficult observing conditions and suggests that it can also be effective for observations low above the horizon. Figure 10E highlights the sensitivity of our detector, which turns out to be comparable or even better than that of a camera with a wide-angle lens. The meteor shown is difficult to visually identify in the image, while the signal from the photodiode is clearly visible above the background noise. This comparison shows the advantages of our approach, which allows us to detect even faint and hard-to-see objects. Figure 10F shows a situation in which more than half of the frame is obscured by clouds. Despite this, a very bright meteor is clearly visible on our detector. This observation indicates the potential of our method in difficult weather conditions and highlights its usefulness in automatic meteor detection. In addition, the two distinct brightness peaks recorded can provide information on the meteor's velocity, a valuable addition to the observational data.