A near-solar-region photoelectric telescope detection twin system and method

Abstract

The application provides a near-solar region photoelectric telescope detection twin system and method, which is used for simulating the detection condition of the near-solar region in the field of view of the telescope. The system comprises: a sky background brightness simulation module, which can interact with a photoelectric telescope, a forward scattering type visibility instrument and a sky background radiance measuring instrument, and is used for simulating and generating sky background brightness; a limit detection capability calculation module, which is used for calculating the limit detection capability of the photoelectric telescope under the known external environment and system parameters; and a field of view detection display module, which is used for simulating the distribution condition of the observed target and the stars after the influence of the sky background is eliminated.

Description

Technical Field

[0001] This invention relates to the field of photoelectric detection, specifically to a photoelectric telescope detection twin system and method for the near-solar region. Background Technology

[0002] With the rapid development of aviation technology, human demand for space exploration is gradually increasing. Currently, photoelectric telescopes, as crucial instruments for photoelectric tracking and measurement, are particularly important. However, for daytime exploration, the detection capability of photoelectric telescopes is reduced due to the influence of complex and strong skylight background brightness. This reduces the observable time for targets, significantly decreasing observation opportunities, effective observation data, and the telescope's overall efficiency. The main interferences for daytime exploration come from the complex atmospheric environment and solar scattering. For distant solar regions, the skylight background brightness can be approximated as a constant value, but for near-solar regions, the skylight background brightness undergoes complex changes with location. Studying near-solar regions and constructing a photoelectric telescope detection model for these regions can help solve the problems of difficult and inefficient daytime exploration.

[0003] In the context of the rapid development of digital technology, new demands have been placed on the digitization level of photoelectric telescopes. Constructing digital twin systems for photoelectric telescopes to improve their digitization level has gradually become a focus of current technological exploration. The construction of a detection twin system for photoelectric telescopes has the following main implications for photoelectric telescope systems:

[0004] Before the detection mission is carried out, the detection situation of the telescope is predicted in advance by inputting simulated atmospheric environment parameters and telescope system parameters, simulating the detection situation of photoelectric telescope, preventing and solving problems that will be encountered during the detection, and assessing the feasibility of the mission.

[0005] During the detection mission, the system interacts with the physical telescope to reflect the telescope's real-time operating status and improve the overall digitalization and intelligence level of the telescope's detection capabilities.

[0006] After the mission is completed, the experimental data generated will be further analyzed to understand its physical significance. This will provide strong support for further research on the changes in telescope detection parameters and physical laws, assess the operational status of the telescope equipment, and facilitate the full life cycle management of the telescope equipment.

[0007] In summary, constructing a detection twin system for near-solar region photoelectric telescopes can effectively solve the problems of insufficient digitization of current photoelectric equipment, difficulty in obtaining sky background brightness, especially in near-solar regions, and the impact of complex sky background brightness variations on detection efficiency during daytime detection. This can strongly promote the execution of photoelectric detection missions. Summary of the Invention

[0008] The technical problem to be solved by this invention is: to address the difficulties in detection by photoelectric telescopes in the near-solar region, and to simulate the detection situation within the field of view of the telescope, a detection twin system model for photoelectric telescopes in the near-solar region is provided.

[0009] The technical solution adopted in this invention is: a near-solar region photoelectric telescope detection twin system, comprising: a sky background brightness simulation module, a limit detection capability calculation module, and a field of view detection display module;

[0010] The sky background brightness simulation module is used to simulate the sky background brightness in the near-sun area and the entire sky on the same day.

[0011] The limit detection capability calculation module is used to calculate the limit detection capability of the photoelectric telescope under known external environment and photoelectric telescope system parameters.

[0012] The field-of-view detection and display module is used to simulate the distribution of observation targets and stars after eliminating the influence of skylight background.

[0013] This invention also proposes a method for detecting twins using a photoelectric telescope in the near-solar region, comprising the following steps:

[0014] S1, the sky background brightness simulation module measures the atmospheric extinction coefficient using a forward-scattering visibility meter. The sky background radiance was measured at a fixed point using a sky background radiance meter. The brightness of the sky background in the near-solar region was calculated. ;

[0015] S2, Limit Detection Capability Calculation Module Based on Skylight Background Brightness The parameters of the photoelectric telescope system are used to determine the limits of its detection capability in the near-solar region.

[0016] S3, the field-of-view detection and display module, is based on the photon count calculation in the limit detection capability calculation module. It simulates the distribution of observation targets and stars in the near-solar region after eliminating the influence of the sky background, and completes the simulation of the telescope's field-of-view detection.

[0017] In summary, compared with the prior art, the photoelectric telescope detection twin system and method for the near-solar region provided by the present invention has the following advantages:

[0018] The algorithm of this invention is computationally simple and can be used for pre-mission mission prediction, in-mission status monitoring, and post-mission data processing of photoelectric telescopes. The detection twin system model of the photoelectric telescope can be used for pre-mission prediction and feasibility assessment; for virtual-real interaction during mission execution, real-time monitoring and reflection of the photoelectric detection system's operational equipment; and for post-mission data processing, in-depth analysis of its physical meaning and parameter change patterns, facilitating the full lifecycle management of the equipment. Constructing a detection twin system model for near-solar region photoelectric telescopes is of great significance for improving the digitization and intelligence levels of photoelectric telescopes and facilitating the full lifecycle management of the equipment. Attached Figure Description

[0019] Figure 1 This is a schematic diagram of the structural composition of a detection twin system;

[0020] Figure 2 This is a flowchart of a method for detecting twins. Detailed Implementation

[0021] To make the objectives, technical solutions, and advantages of this invention clearer, the invention will be further described in detail below with reference to the accompanying drawings and embodiments. It should be understood that the specific embodiments described herein are merely illustrative and not intended to limit the invention. Furthermore, the technical features involved in the various embodiments of this invention described below can be combined with each other as long as they do not conflict with each other. To achieve the above objectives, this invention adopts the following technical solution.

[0022] This invention provides a near-solar region photoelectric telescope detection twin system, such as... Figure 1 As shown, the system includes: a sky background brightness simulation module, a limit detection capability calculation module, and a field-of-view display module. The sky background brightness simulation module includes a forward-scattering visibility meter and a sky background radiance meter, used to generate the sky background brightness in the near-solar region and the entire sky. The limit detection capability calculation module consists of a photoelectric telescope and a computer, used to generate the limit detection capability of the photoelectric telescope in the near-solar region based on the sky background brightness in the near-solar region and the system's own parameters. The field-of-view display module, based on the photon number calculation in the limit detection capability calculation module, simulates the distribution of observed targets and stars after eliminating the influence of the sky background.

[0023] Based on the aforementioned near-solar region photoelectric telescope detection twin system, this invention also provides a method for near-solar region photoelectric telescope detection twins, such as... Figure 2 As shown, it includes the following steps: S1, the sky background brightness simulation module measures the atmospheric extinction coefficient using a forward scattering visibility meter. The sky background radiance was measured at a fixed point using a sky background radiance meter. The brightness of the sky background in the near-solar region was calculated. S2, the limit detection capability calculation module, obtains the limit detection capability of the near-solar region based on the brightness of the sky background and the parameters of the photoelectric telescope system; S3, the field of view detection display module, based on the photon number calculation in the limit detection capability calculation module, simulates the distribution of observation targets and stars in the near-solar region after eliminating the influence of the sky background, and completes the simulation of the telescope's field of view detection.

[0024] In step S1, specifically, the theoretical position of the solar target in the navigation reference coordinate system is first obtained. , These are the azimuth and elevation angles, respectively, determined by the azimuth and elevation angles of the telescope's observation direction. The angle between the observation direction and the direction of solar incidence is obtained. :

[0025] (1)

[0026] Considering Rayleigh and Mie scattering occurring in the atmosphere, the overall scattering equation is obtained. :

[0027] (2)

[0028] According to the zenith angle of the sun Observing the zenith angle with a telescope The optical path caused by atmospheric scattering is obtained. and :

[0029] (3)

[0030] (4)

[0031] Based on the sun's brightness Atmospheric extinction coefficient measured by a forward-scattering visibility meter The brightness of the sky background is obtained by combining equations (2), (3), and (4). :

[0032] (5)

[0033] Use a sky background radiance meter to obtain the sky background luminance at a fixed point. and with In comparison, the fitting coefficients were obtained. and final sky background brightness :

[0034] (6)

[0035] (7)

[0036] Furthermore, the sky background brightness is obtained from the sky background brightness simulation module. The limit detection capability calculation module in step S2 is used to obtain the system parameters of the photoelectric telescope itself and the external environmental parameters: dark current electron noise. Reading out electronic noise The quantum efficiency of the detector for the background light of the sky Planck constant Speed ​​of light Average wavelength The area of ​​a single pixel of the detector Exposure time Average transmittance of optical system Primary mirror obstruction ratio ; Optical system aperture ; focal length of optical system ; Spectral filtering affects the background spectral transmittance coefficient Calculate background signal photoelectron noise :

[0037] (8)

[0038] Based on the photon flux density of 0 magnitude stars Starlight Atmospheric average transmittance Photoelectric telescope system parameters: the detector's quantum efficiency towards the target. The number of pixels occupied by the observed target ; Spectral filtering affects the target spectral transmittance coefficient Calculate the number of photoelectrons in the starlight signal :

[0039] (9)

[0040] Based on the telescope's detection signal-to-noise ratio threshold Equations (8) and (9) are used to calculate the maximum magnitude of stars that can be detected by photoelectric telescopes. :

[0041] (10)

[0042] Based on environmental parameters: Boltzmann constant The temperature of the sun's blackbody average wavelength Surface area of ​​the sun Average distance between the Earth and the Sun ,calculate ~ Wavelength, solar irradiance on space targets :

[0043] (11)

[0044] Based on the effective reflective area of ​​the space target The average reflectivity of the target surface The angle between the direction of sunlight incident and the direction of the normal to the target surface The angle between the line connecting the detector and the target and the direction of the normal to the space target. Distance between the target and the photoelectric telescope system The quantum efficiency of the detector on the target The number of photoelectrons received by each pixel of the detector is calculated as follows: :

[0045] (12)

[0046] Calculate the detection limit distance based on equations (11) and (8). :

[0047] (13)

[0048] Based on the photon number calculation in the aforementioned limit detection capability calculation module, the distribution of observation targets and stars in the near-solar region after eliminating the influence of skylight background is simulated to complete the simulation of the telescope's field of view detection. Step S3 includes the following steps:

[0049] For stellar observation targets, according to equation (9) and the limit for probing star magnitudes... Calculate its starlight photon number :

[0050] (14)

[0051] Select the number of photons corresponding to the brightest observed object within the field of view. Record its grayscale as ;

[0052] Setting the background brightness grayscale value to 0, for a photon number in the field of view of... Gray value distribution of any observed target :

[0053] (15)

[0054] In summary, compared with the prior art, the near-solar region photoelectric telescope detection twin system and method provided by the present invention have the following advantages: the algorithm of the present invention is simple to calculate and can be used for pre-mission prediction, in-process status monitoring and post-mission data processing of photoelectric telescopes.

Claims

1. A method for detecting twins using a photoelectric telescope in the near-solar region, characterized in that, Includes the following steps: S1, the sky background brightness simulation module measures the atmospheric extinction coefficient using a forward-scattering visibility meter. The sky background radiance was measured at a fixed point using a sky background radiance meter. The brightness of the sky background in the near-solar region was calculated. ; S2, Limit Detection Capability Calculation Module Based on Skylight Background Brightness The parameters of the photoelectric telescope system are used to determine the limits of its detection capability in the near-solar region. S3. The field-of-view detection and display module, based on the photon number calculation in the limit detection capability calculation module, simulates the distribution of observation targets and stars in the near-solar region after eliminating the influence of skylight background, thus completing the simulation of the telescope's field-of-view detection. Step S1 includes the following steps: S11. Obtain the theoretical position of the solar target in the navigation reference coordinate system. Based on the azimuth and elevation angles of the telescope's observation direction, obtain the angle between the observation direction and the solar incident direction. S12. Considering Rayleigh and Mie scattering occurring in the atmosphere, the total scattering equation is obtained; S13. Based on the brightness of the sun itself, the angle between the observation direction and the direction of the sun's incidence, the atmospheric extinction coefficient measured by the forward scattering visibility meter, and the total scattering equation, the brightness of the sky background in the near-sun region is obtained. S14. Use a sky background radiance meter to obtain the sky background brightness at a fixed point, and compare it with the calculated sky light background brightness in the near-solar region to obtain the fitting coefficient and the final sky background brightness. Step S2 includes the following steps: S21. Based on the sky background brightness, obtain the system parameters of the photoelectric telescope itself and the external environment parameters, and calculate the background signal photoelectron noise; S22. Calculate the number of photoelectrons in the starlight signal based on the star background brightness parameters and the parameters of the photoelectric telescope system. S23. Calculate the ultimate magnitude of the photoelectric telescope based on the detection signal-to-noise ratio threshold, background signal photoelectron noise, and the number of photons of the detected target. S24. Calculate the solar irradiance on space targets in a specific detection band based on real-time or predicted environmental parameters. S25. Based on the space target detection data and telescope system parameters, calculate the number of photoelectrons received by each pixel of the detector; S26. Calculate the detection limit distance based on the solar irradiance on the space target and the number of photoelectrons received by each pixel.

2. The method for detecting twins using a photoelectric telescope in the near-solar region as described in claim 1, characterized in that, Step S3 includes the following steps: S31. For stellar observation targets, calculate the number of starlight photons of the stellar observation target based on the ultimate detection magnitude; S32. Select the number of photons corresponding to the brightest observed object within the field of view, and record its gray level as... ; S33. Set the background brightness grayscale value to zero, and obtain the number of photons in the field of view as follows: Gray value distribution of any observed target .

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