Parallax observations from adjacent CCDs have been applied to detect satellite jitter, and the highest detectable jitter frequency reaches up to half CCDs image line frequency, among which, however, not all frequencies’ jitter could be detected accurately. Jitter error mainly comes from the noise in offset data. In this research, it is found that at some frequencies the noise is amplified significantly, leading to seriously deviated jitter components and even unreliable jitter results. This research focuses on the noise-amplifying questions in jitter detection and explores what CCD parameters determine them. Firstly, the error transfer coefficients (ETC) between jitter and offset is derived, and the frequencies are divided into three categories: blind frequencies, noise-amplifying frequencies and noise-suppressing frequencies. Secondly, for two adjacent CCDs, formulas are established to determine their blind frequencies and noise-amplifying bands, which indicate that it is the two CCDs’ image line time ${\mathit{t}}_{\mathrm{r}}$ and the distance l between the two CCDs’ first lines that determine their blind frequencies and noise-amplifying bands. The reciprocal of the product of ${\mathit{t}}_{\mathrm{r}}$ and l is defined as the fundamental frequency F of the CCD pair. As a result, the blind frequencies and noise-amplifying bands both reoccur with a period of fundamental frequency F, but unlike those isolated bind frequencies, the noise-amplifying bands span much wider, up to nearly 1/3 jitter bandwidth. Thirdly, for three adjacent CCDs forming two CCD pairs, aliasing between the two pairs’ noise-amplifying bands is first proven to be inevitable and reoccurs in cycles. Formulas are then established to extract the aliasing components and compute the aliasing period length. Experiments and simulations are conducted to test the constructed theories. Results show that the RMSE is 7.127 $\times 10^{-5}\mathrm{Hz}$ for blind frequencies formulas, and the RRMSEs are 0.0051% for noise-amplifying bands’ period formulas, 0.0033% for aliasing period, and 1.2610% for noise-amplifying bandwidth, proving that the established formulas could generate reliable results for the blind frequencies, noise-amplifying bands and their aliasing components of three adjacent CCDs. Our studies are expected to help analyze more CCDs’ noise-amplifying problems and provide a prospect to reduce their impact on jitter detection by optimizing CCD parameter values.

相邻CCD的视差观测已被用于检测卫星抖动，可检测的最高抖动频率可达CCD图像行频的一半，但并非所有频率的抖动都能准确检测。抖动误差主要来自偏移数据中的噪声。在本次研究中发现，在某些频率下，噪声被显着放大，导致抖动分量严重偏差，甚至抖动结果不可靠。这项研究的重点是抖动检测中的噪声放大问题，并探讨了哪些 CCD 参数决定了这些问题。首先推导出抖动和偏移之间的误差传递系数（ETC），将频率分为盲频率、噪声放大频率和噪声抑制频率三类。其次，${\mathit{吨}}_{\mathrm{r}}$两个 CCD 的第一条线之间的距离l决定了它们的盲频率和噪声放大带。产品的倒数${\mathit{吨}}_{\mathrm{r}}$和升的定义为基本频率˚F所述CCD对。结果，盲频率和噪声放大频带都以基频F的周期重新出现，但与那些孤立的绑定频率不同，噪声放大频带的跨度要宽得多，高达近 1/3 的抖动带宽。第三，对于形成两个 CCD 对的三个相邻 CCD，首先证明两对噪声放大带之间的混叠是不可避免的，并且会循环出现。然后建立公式以提取混叠分量并计算混叠周期长度。进行实验和模拟以测试构建的理论。结果显示 RMSE 为 7.127 $\times 10^{-5}\mathrm{赫兹}$对于盲频公式，噪声放大频带的周期公式的 RRMSE 为 0.0051%，混叠周期的 RRMSE 为 0.0033%，噪声放大带宽的 RRMSE 为 1.2610%，证明所建立的公式可以为盲频、噪声- 三个相邻 CCD 的放大带及其混叠分量。我们的研究有望帮助分析更多 CCD 的噪声放大问题，并为通过优化 CCD 参数值来减少它们对抖动检测的影响提供前景。