Imaging method and imaging system for performing in-orbit geometric calibration through star observation
A technology of geometric calibration and imaging method, which is applied in the direction of navigation, measuring devices, instruments, etc. through velocity/acceleration measurement, to overcome the problem of weak geometric strength, improve the geometric strength of measurement, and achieve the effect of high signal-to-noise ratio
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specific Embodiment approach 1
[0024] Specific implementation mode 1. Combination figure 1 To illustrate this embodiment, the system for on-orbit geometric calibration through stargazing mainly includes satellite platforms, star sensors, line array cameras and gyroscopes. The star sensor, line array camera and gyroscope are all installed on the satellite platform. The star sensor measures the on-orbit attitude of the satellite, and the gyroscope outputs the angular velocity output by the satellite.
[0025] m V The illuminance produced by the magnitude outside the atmosphere is:
[0026]
[0027] where E 0 =2.54×10 -6 lux, is the illuminance of a zero-magnitude star outside the atmosphere, and lux is the unit of illuminance; MV Represents the star magnitude.
[0028] require M V The magnitude of the light at the detector integration time t int The number of starlight charges that may be generated on a single pixel cannot reach the full well charge of the detector, and the signal-to-noise ratio can...
specific Embodiment approach 2
[0046] Specific embodiment 2. This embodiment is the imaging method of the on-orbit geometric calibration system through stargazing described in specific embodiment 1. This method adopts the combined stargazing mode of star sensitivity + gyroscope. First, the imaging method of the line array camera The selection of parameters requires that the focal ratio of the optical system of the line scan camera and 2.44 times the central wavelength be greater than the pixel size, expressed as:
[0047] 2.44λF>a
[0048] Where λ is the average light wavelength.
[0049] Secondly, according to the magnitude of the predicted star and the spectral range of the detector, set an appropriate integration time to ensure that the linear array detector is not saturated and the signal-to-noise ratio is greater than or equal to 2; namely:
[0050] set M V The magnitude of the light at the detector integration time t int The number of starlight charges that may be generated on a single pixel cannot...
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