Daytime star measuring device of hybrid star sensor

Abstract

The invention discloses a hybrid star sensor daytime star measuring device, which relates to the technical field of celestial navigation, and comprises a star measuring assembly, a two-dimensional fast reflector, a control circuit board and a shell, all the parts are integrally installed on the shell, the satellite measuring assembly is arranged in the shell and comprises a telephoto lens, a multi-band-pass satellite observation window and a satellite measuring camera, reflected light rays are converged on the satellite measuring camera arranged behind the telephoto lens through the telephoto lens, the multi-band-pass satellite observation window is arranged between the telephoto lens and the satellite measuring camera and divided into a plurality of areas, and the satellite measuring camera is arranged in the shell. Only light of different specific wavebands can pass through each region, and the light is moved to the optimal region of the multi-band-pass star observation window by combining small-angle adjustment of the reflector, so that rapid selection of the wavebands is realized; the two-dimensional fast reflecting mirror and the satellite measuring assembly are coaxially arranged, the projection position is rotated and offset through two-axis control, and the small view field is expanded into the large view field by fast rotation and image splicing. The device solves the problem of background saturation of satellite measurement in the atmosphere in the daytime, and improves the signal-to-noise ratio and the adaptability.

Description

Technical Field

[0001] This invention relates to the technical field of astronomical navigation, and more specifically, to a hybrid star sensor daytime star measurement device. Background Technology

[0002] Celestial navigation, also known as star navigation, observes stars through star sensors to provide fully autonomous, interference-resistant, and high-precision attitude information or star measurement vector information for long-endurance missions of various platforms. It has the advantages of strong autonomy, resistance to electromagnetic interference, and anti-spoofing, and can effectively suppress the long-term accuracy drift error of inertial navigation systems. Celestial navigation is widely used in various platforms and is a fundamental device for various platforms to safely achieve their missions.

[0003] The application of astronomical navigation technology to various platforms within the atmosphere first requires solving the problem of daytime star measurement. Currently, some platforms equipped with astronomical navigation systems within the atmosphere employ daytime star measurement technology using small-field-of-view star sensors with a field of view of less than 1°. This technology uses a long-focal-length, large-aperture star measurement optical system based on a dual-axis tracking system. It has strong resistance to stray light and is a mature technology. The background intensity of star measurement caused by factors such as high-temperature gas luminescence and atmospheric background radiation is two to three orders of magnitude lower than that of large-field-of-view star sensors (inversely proportional to the square of the F number). However, it suffers from problems such as large system size and weight, poor adaptability under limited space constraints, the need for multiple star measurements, and slow response speed. In contrast, the large-field-of-view star sensor daytime star measurement technology, mainly used outside the atmosphere, generally adopts a large-field-of-view design of 5° or more. A single star measurement can obtain the results of multiple star measurements from small-field-of-view astronomical navigation systems, offering advantages such as small size and weight, high accuracy, and high reliability. However, due to the strong atmospheric background radiation during the day in the atmosphere, and the possibility of high-temperature gas luminescence near the star sensor's observation window under high-speed flight conditions, the background image of the large field of view star measurement during the day in the atmosphere will be fully or partially saturated, making it extremely difficult for the large field of view star sensor to measure stars during the day. Summary of the Invention

[0004] The purpose of this invention is to address the problems of existing small-field-of-view star sensors, such as large size and weight, poor adaptability, and slow response speed, as well as the poor anti-stray light capability and poor daytime star measurement capability of large-field-of-view star sensors. Based on the existing daytime star measurement technology of small-field-of-view star sensors, this invention provides a hybrid star sensor daytime star measurement technology that comprehensively suppresses the influence of various stray lights in the atmosphere on star sensor measurement, realizes a lightweight hybrid star sensor daytime star measurement technology solution, meets the needs of various platforms in the atmosphere for high-precision attitude measurement information, and solves the problem of lightweight daytime star measurement in the atmosphere.

[0005] The technical solution of the present invention is: to provide a hybrid star sensor daytime star measurement device, the device comprising: a star measurement component, a two-dimensional fast reflector, a control circuit board and a housing;

[0006] The housing is a structural component that integrates the star-measuring assembly, the two-dimensional fast reflector, and the control circuit board. The star-measuring assembly is located inside the housing, and the two-dimensional fast reflector is also located inside the housing and arranged coaxially with the star-measuring assembly. The housing has an opening above the two-dimensional fast reflector to allow light to enter. The control circuit board is externally mounted on the housing and is connected to the star-measuring assembly and the two-dimensional fast reflector via cables. The control circuit board receives images acquired by the star-measuring assembly and transmits them to the outside for analysis. The control circuit board also sends rotation control commands to the two-dimensional fast reflector to rotate it by a certain angle.

[0007] The star-measuring assembly includes a star-measuring camera, a multi-bandpass observation window, and a telephoto lens. The telephoto lens is located on the opposite side of the two-dimensional fast reflector, converging the reflected light onto the star-measuring camera positioned behind the telephoto lens. A multi-bandpass observation window is positioned between the star-measuring camera and the telephoto lens. The multi-bandpass observation window is divided into several regularly shaped regions, each of which is coated with a filter film of completely different specifications. The filter film only allows light of a specific wavelength to pass through. The light selects different positions of the multi-bandpass observation window to pass through and is imaged on the star-measuring camera, enabling rapid selection of the working wavelength.

[0008] The two-dimensional fast reflector includes a reflector, a control circuit, and two control axes. The reflector is a circular plane mirror. Both control axes are located on the back edge of the reflector. The control circuit rotates the control command and drives the reflector to rotate within a small angle range by controlling the extension and retraction of the two control axes. When rotating, the tilt angle of the reflector surface changes, causing the reflection direction of the incident light to shift, thus moving the image point between different regions on the multi-bandpass observation window.

[0009] The two-dimensional fast reflector performs a wide-range scan. The frame-by-frame images acquired by the satellite measurement component are output to the outside via a control circuit board. The external system stitches these frame-by-frame images into a large field-of-view image. The stitching logic is as follows: the two-dimensional fast reflector has a stable scanning speed. Based on the total number of frames acquired, the position of each frame in the large field-of-view image is deduced. The overlapping parts are then image-synthesized by averaging the gray values.

[0010] In any of the above technical solutions, the surface of the shell is further subjected to black oxidation treatment, and the inner surface through which the light path passes is sprayed with matte paint.

[0011] In any of the above technical solutions, the telephoto lens is further designed with a large F-number.

[0012] In any of the above technical solutions, the two control axes of the two-dimensional fast reflector are not set on the same diameter of the reflector.

[0013] In any of the above technical solutions, the multi-bandpass stargazing window is further composed of multiple filters spliced ​​together. Each filter is a square lens and is coated with a filter film that allows the corresponding working band to pass through while cutting off other bands.

[0014] In any of the above technical solutions, the multi-bandpass stargazing window is further defined as a square lens, with different working bandpass filter films coated on different areas of its surface.

[0015] In any of the above technical solutions, the measurement process of the device for measuring a single star during the day is as follows: the star sensor controls the rotation of the two-dimensional fast reflector through the control circuit board to capture the star image; after the star enters the field of view, the star measurement component completes the acquisition of the star's optical image. Among them, based on the comparison between the grayscale of the real-time acquired image and the preset threshold, it is determined whether the star's projected light passes through a suitable multi-bandpass star observation window. If it is not suitable, the star sensor controls the two-dimensional fast reflector to rotate slightly through the control circuit board, changes to another position, and judges again until the grayscale of the real-time acquired image meets the requirements. The acquired clear and easy-to-judge image is transmitted to the outside after simple noise reduction and optical correction for analysis and calculation.

[0016] In any of the above technical solutions, further, when the device performs multi-star synchronous acquisition during the day, the working process is as follows: the star sensor controls the two-dimensional fast reflector to rotate rapidly through the control circuit board, sweeping across a large field of view in a short time, and outputs the frame-by-frame images acquired during this period. After external processing, the images are stitched together to form a large field of view image. The stitching process is as follows: based on the total number of frames of the acquired images, the position of each frame image in the large field of view image is deduced, and the overlapping parts are image synthesized by averaging the gray values, thus completing the star search and tracking within the large field of view range.

[0017] The beneficial effects of this invention are:

[0018] The technical solution in this invention achieves rapid search and tracking of multiple stars within a wide field of view through the coordinated operation of a rapidly and accurately rotating two-dimensional fast-reflecting mirror and a star-measuring component with multiple bandpass observation windows. This is equivalent to the multi-star synchronous measurement effect of a large field-of-view star sensor, while retaining the background stray light suppression capability brought by the long focal length and high F-number design with a small field of view. It solves the defects of poor anti-stray light capability and poor daytime star measurement capability. By using multiple bandpass observation windows to further subdivide the working band, combined with the small-angle range tracking adjustment of the two-dimensional fast-reflecting mirror, it achieves rapid online switching and selection of narrow-band working bands, further ensuring that the star measurement background is unsaturated in the daytime environment within the atmosphere, improving the signal-to-noise ratio of star measurement during the day, and achieving stable detection and tracking of star targets.

[0019] Furthermore, this invention is a novel daytime star measurement scheme that combines the advantages of a small field-of-view star sensor with strong daytime star measurement capabilities, as well as the ability of a large field-of-view star sensor to measure multiple star targets simultaneously. It fully meets the needs of various platforms within the atmosphere for fully autonomous, interference-resistant, and high-precision attitude measurement information, and is a feasible solution to the problem of daytime star measurement within the atmosphere. Attached Figure Description

[0020] The advantages of the above and additional aspects of the present invention will become apparent and readily understood in the description of the embodiments in conjunction with the following drawings, wherein:

[0021] Figure 1 This is a schematic diagram of the composition of a hybrid star sensor daytime star measurement device according to an embodiment of the present invention;

[0022] Figure 2 This is a schematic block diagram of the internal components of a hybrid star sensor daytime star measuring device according to an embodiment of the present invention;

[0023] Figure 3 This is a schematic diagram of a multi-band star-observing window of an embodiment of a hybrid star sensor daytime star-measuring device according to an embodiment of the present invention;

[0024] Figure 4 This is a schematic diagram of a multi-band star-observing window of another embodiment of a hybrid star sensor daytime star-measuring device according to one embodiment of the present invention;

[0025] Figure 5 This is a schematic diagram of a two-position fast-reflecting mirror of a hybrid star sensor daytime star measurement device according to an embodiment of the present invention;

[0026] Figure 6 This is a conceptual schematic diagram of the equivalent large field of view of a hybrid star sensor daytime star measuring device according to an embodiment of the present invention.

[0027] Among them, 1-star measuring component, 2-two-dimensional fast reflector, 3-control circuit board, 4-housing, 21-reflector, 22-control axis. Detailed Implementation

[0028] To better understand the above-mentioned objectives, features, and advantages of the present invention, the present invention will be further described in detail below with reference to the accompanying drawings and specific embodiments. It should be noted that, unless otherwise specified, the embodiments of the present invention and the features thereof can be combined with each other.

[0029] In the following description, many specific details are set forth in order to provide a full understanding of the invention. However, the invention may also be practiced in other ways different from those described herein, and therefore the scope of protection of the invention is not limited to the specific embodiments disclosed below.

[0030] like Figure 1 As shown, this embodiment provides a hybrid star sensor daytime star measurement device, which includes: a star measurement component 1, a two-dimensional fast reflector 2, a control circuit board 3, and a housing 4.

[0031] The housing 4 is a structural component that integrates the star measuring component 1, the two-dimensional fast reflector 2, and the control circuit board 3. The star measuring component 1 is placed inside the housing 4, and the two-dimensional fast reflector 2 is set inside the housing 4 and arranged coaxially with the star measuring component 1. The housing 4 has an opening above the two-dimensional fast reflector 2 to allow light to enter.

[0032] The control circuit board 3 is mounted on the housing 4 and connected to the satellite measuring component 1 and the two-dimensional fast reflector 2 via a cable. The control circuit board 3 receives the images collected by the satellite measuring component 1 and transmits them to the outside for analysis. The control circuit board 3 sends rotation control commands to the two-dimensional fast reflector 2 to make it rotate by an angle.

[0033] The housing 4 is made of materials such as aviation aluminum or Invar steel, and the surface is treated with black oxidation. The inner surface through which some light passes is sprayed with matte paint to achieve the function of absorbing stray light.

[0034] like Figure 2 As shown, the star-measuring component 1 includes a star-measuring camera, a multi-bandpass observation window, and a telephoto lens. The telephoto lens adopts an integrated structure combining a Cassegrain primary and secondary mirror with a compensation lens group to achieve a lightweight and compact design. While ensuring a large aperture to improve star-measuring capabilities, it is also designed with a large F-number (F-number means the ratio of equivalent focal length to optical aperture, which is a technical term in this field) to achieve better background stray light suppression capabilities.

[0035] The satellite camera selects working bands such as visible light, short-wave infrared, or ultraviolet based on the spectral characteristics of the observed target star and the main background stray light in order to achieve a better signal-to-noise ratio for daytime satellite measurements.

[0036] A multi-bandpass observation window is placed between the star-measuring camera and the telephoto lens to further subdivide the working band of the star sensor. Combined with the small-angle range tracking and adjustment of the two-dimensional fast reflector, it enables rapid selection of the working band and further improves the signal-to-noise ratio of star measurement during the day.

[0037] Specifically, the multi-bandpass observatory is divided into several regularly shaped regions, each with a filter film of completely different specifications coated on it. The filter film only allows light of specific wavelengths to pass through. The light selects different positions of the multi-bandpass observatory to pass through and is imaged on the star-measuring camera, enabling rapid selection of the working wavelength.

[0038] The two-dimensional fast reflector 2 is coaxially arranged with the star-measuring component 1, and the two-dimensional fast reflector 2 is tilted at a certain angle to the horizontal plane, such as... Figure 5As shown, the two-dimensional fast reflector assembly 2 includes a reflector 21, a control circuit, and two control shafts 22. The reflector 21 is a circular plane mirror. Both control shafts 22 are located at the back edge of the reflector 21, but they are not located on the same diameter of the reflector 21. The control circuit provides rotation control commands, which drive the reflector 21 to rotate within a small angle range by controlling the extension and retraction of the two control shafts 22. When rotating, the tilt angle of the reflector 21 changes, causing the reflection direction of the incident light to shift, thereby moving the projection position of the starlight image point on the star measuring assembly 1.

[0039] Because the instantaneous field of view is small and the projection area is limited, the light cannot cover the entire area of ​​the multi-bandpass star window at once. It usually only covers one or a few grids of the window. When the reflector does not rotate, the light path is fixed, and the star image is projected onto a specific position of the multi-bandpass star window, corresponding to a fixed narrow band of the window. If it is necessary to switch to other areas, the system can make a small angle adjustment by controlling the reflector to slightly shift the projected image point, thereby moving it to an adjacent grid, ensuring that the starlight passes through the optimal filtering area and avoiding background saturation.

[0040] like Figure 3 The image shows one embodiment of the working window of a multi-bandpass satellite sensor covering the 0.2-0.6μm working band. The window consists of multiple filters fixed by a structural component. The structural component is about the same size as the detector and is fixed in front of the detector. Each filter is about 4mm × 4mm in size and is coated with a filter film that allows the corresponding working band to pass through while blocking other bands. Light of different frequency bands will pass through different filters. Figure 3 The display shows a 3×3 grid layout, with bands labeled from top left to bottom right as 0.2-0.3μm, 0.3-0.4μm, 0.4-0.5μm, and 0.5-0.6μm, respectively, in a gradient from dark gray to light blue. A star in the center grid indicates a typical projection position. By adjusting the small angle of the two-dimensional fast-reflecting mirror, starlight can be projected onto specific grids, enabling rapid switching of narrowband operating wavelengths. This ensures that the background radiation during daytime atmospheric radiation and high-temperature gas luminescence remains unsaturated, achieving stable detection and tracking of celestial targets.

[0041] During daytime star measurements, if strong background radiation in the current band causes image saturation, a small-angle tracking adjustment using a two-dimensional fast reflector projects starlight onto adjacent grid cells, selecting the narrowest band with the highest signal-to-noise ratio. This is an online, rapid switching selection mechanism that further ensures unsaturated background radiation during star measurements, improving the signal-to-noise ratio for daytime measurements. Compared to existing static filtering, this achieves adaptive spectral band optimization.

[0042] like Figure 4As shown, this is another implementation of the working window of a multi-bandpass satellite sensor covering the 0.6-1.6μm working band. Different working bandpass filters are deposited on different areas of the imaging detector protective glass to achieve the function of multiple working bandpasses. Figure 4 The image displays a cross-shaped layout, with the central circle labeled 0.6-0.8 μm and the surrounding four quadrants labeled 0.8-1.0 μm, 1.0-1.2 μm, 1.2-1.4 μm, and 1.4-1.6 μm. This is achieved by comparing... Figure 3 A similar adjustment mechanism can dynamically select the optimal band to further improve the signal-to-noise ratio.

[0043] like Figure 6 As shown, due to the extremely fast response and rotation speed of the two-dimensional fast reflector, after scanning a wide area and acquiring multiple frames of images, it can output to the outside and expand the 3° instantaneous small field of view to a large field of view of about 12°×12° through image stitching. This method retains the advantage of strong star measurement capability in a small field of view and can also achieve the effect of equivalent large field of view multi-star measurement. At the same time, combined with multi-bandpass star observation windows, it can realize rapid switching of narrowband working bands, ensuring that the star measurement background is unsaturated under daytime atmospheric background radiation and high-temperature gas luminescence environment. It can also further control the star target staring of the two-dimensional fast reflector to improve the star measurement signal-to-noise ratio.

[0044] The stitching logic of the above image stitching is as follows: because the scanning speed of the two-dimensional fast reflector 2 is stable, the moving interval of the center point of the adjacent frame image is fixed, and the large field of view range of the captured image is also determined. The moving interval of the center point of the adjacent frame image can be calculated by the total number of frames. All frames are placed in the correct position in the large field of view image. The image of the overlapping part of the image is synthesized by averaging the gray values ​​to obtain the stitched large field of view image.

[0045] In practical engineering, this is a solution to address pain points. Traditional small field-of-view star sensors have strong anti-stray light capabilities, but measuring multiple stars requires moving the entire device or performing multiple scans, resulting in slow measurement speed. Furthermore, due to their large size, small field-of-view star sensors are not suitable for moving equipment in confined spaces. On the other hand, large field-of-view star sensors, although small in size and with a large field of view, can measure multiple stars simultaneously, but the background is too strong during the day, resulting in high saturation and making measurement difficult.

[0046] The hybrid star sensor daytime star measurement device proposed in this invention has the advantages of strong daytime star measurement capability of small field-of-view star sensors and the characteristics of simultaneous measurement of multiple star targets of large field-of-view star sensors. Its adaptability is also greatly improved. It is an original and novel daytime star measurement scheme and a feasible solution for the problem of daytime star measurement within the atmosphere.

[0047] The working process of the hybrid star sensor daytime star measurement device provided by this invention is as follows: During the star measurement process, the star sensor controls the rotation of the two-dimensional fast reflector through the control circuit board to capture star images; after the star enters the field of view, the star measurement component completes the acquisition of the star's optical image, which is then transmitted to the outside after simple noise reduction and optical correction for analysis and calculation; among them, based on the gray level of the real-time acquired image, it is determined whether the star's projected light passes through the appropriate multi-bandpass star observation window. When the gray level is too high and oversaturation occurs, it is difficult to distinguish the star in the image. Therefore, the star sensor controls the two-dimensional fast reflector to rotate slightly through the control circuit board so that the light passes through the appropriate position on the multi-bandpass star observation window to acquire a clear and easily judged image.

[0048] When multi-star synchronous acquisition is required, the two-dimensional fast reflector is driven to rotate rapidly, sweeping across a large field of view in a short time. The frame-by-frame images acquired during this period are output, and after external processing, they are stitched together to form a large field of view image, thus completing the star search and tracking within the large field of view.

[0049] In summary, this invention proposes a hybrid star sensor daytime star measurement device, comprising: a star measurement component 1, a two-dimensional fast reflector 2, a control circuit board 3, and a housing 4.

[0050] The housing 4 is a structural component that integrates the star-measuring assembly 1, the two-dimensional fast reflector 2, and the control circuit board 3. The star-measuring assembly 1 is placed inside the housing 4, and the two-dimensional fast reflector 2 is set inside the housing 4 and arranged coaxially with the star-measuring assembly 1. The housing 4 has an opening above the two-dimensional fast reflector 2 to allow light to enter. The control circuit board 3 is externally mounted on the housing and is connected to the star-measuring assembly 1 and the two-dimensional fast reflector 2 via cables. The control circuit board 3 receives the images collected by the star-measuring assembly 1 and transmits them to the outside for analysis. The control circuit board 3 sends rotation control commands to the two-dimensional fast reflector 2 to rotate it by a certain angle.

[0051] The star measurement component 1 includes a star measurement camera, a multi-bandpass observation window, and a telephoto lens. The telephoto lens is located on the opposite side of the two-dimensional fast reflector 2, and focuses the reflected light onto the star measurement camera located behind the telephoto lens. A multi-bandpass observation window is set between the star measurement camera and the telephoto lens. The multi-bandpass observation window has multiple filters coated with different specifications. The filters only allow light of specific wavelengths to pass through. The light selects different positions of the multi-bandpass observation window to pass through and is imaged on the star measurement camera, realizing rapid selection of the working wavelength.

[0052] The two-dimensional fast reflector 2 includes a reflector 21, a control circuit, and two control axes 22. The reflector 21 is a circular plane mirror. Both control axes 22 are located at the back edge of the reflector. The control circuit rotates the control command and drives the reflector to rotate within a small angle range by controlling the extension and retraction of the two control axes. When rotating, the tilt angle of the reflector 21 changes, causing the reflection direction of the incident light to shift, thus moving the image point to different positions on the multi-bandpass observation window.

[0053] The two-dimensional fast reflector 2 performs a wide-range scanning, and the satellite measurement component 1 collects frame-by-frame images during the process and outputs them to the outside via the control circuit board 3. The external system then stitches the frame-by-frame images into a large field-of-view image.

[0054] The steps in this invention can be adjusted, combined, or deleted according to actual needs.

[0055] The units in the device of the present invention can be merged, divided, or reduced according to actual needs.

[0056] In this invention, the terms "installation," "connection," "linking," and "fixing" should be interpreted broadly. For example, "connection" can be a fixed connection, a detachable connection, or an integral connection; "linking" can be a direct connection or an indirect connection through an intermediate medium. Those skilled in the art can understand the specific meaning of these terms in this invention according to the specific circumstances.

[0057] The shapes of the components in the accompanying drawings are schematic and may differ from their actual shapes. The drawings are only used to illustrate the principles of the present invention and are not intended to limit the present invention.

[0058] Although the invention has been disclosed in detail with reference to the accompanying drawings, it should be understood that these descriptions are merely exemplary and not intended to limit the application of the invention. The scope of protection of the invention is defined by the appended claims and may include various modifications, alterations, and equivalents made to the invention without departing from the scope and spirit of the invention.

Claims

1. A hybrid star sensor daytime star measurement device, characterized in that, The device includes: a star-measuring component (1), a two-dimensional fast reflector (2), a control circuit board (3), and a housing (4); The housing (4) is a structural component that integrates the star measuring component (1), the two-dimensional fast reflector (2), and the control circuit board (3). The star measuring component (1) is placed inside the housing (4), and the two-dimensional fast reflector (2) is set inside the housing (4) and arranged coaxially with the star measuring component (1). The housing (4) has an opening above the two-dimensional fast reflector (2) to allow light to enter. The control circuit board (3) is mounted on the housing and is connected to the star measuring component (1) and the two-dimensional fast reflector (2) via a cable. The control circuit board (3) receives the images collected by the star measuring component (1) and transmits them to the outside for analysis. The control circuit board (3) sends rotation control commands to the two-dimensional fast reflector (2) to make it rotate by an angle. The star measurement component (1) includes a star measurement camera, a multi-bandpass observation window and a telephoto lens. The telephoto lens is located on the opposite side of the two-dimensional fast reflector (2) and converges the reflected light onto the star measurement camera located behind the telephoto lens. A multi-bandpass observation window is set between the star measurement camera and the telephoto lens. The multi-bandpass observation window is divided into several regularly shaped areas. Each area is coated with a filter film of completely different specifications. The filter film only allows light of a specific wavelength to pass through. The light selects different positions of the multi-bandpass observation window to pass through and is imaged on the star measurement camera, so as to realize the rapid selection of the working wavelength. The two-dimensional fast reflector (2) includes a reflector (21), a control circuit and two control axes (22). The reflector (21) is a circular plane mirror. Both control axes (22) are located at the back edge of the reflector. The control circuit rotates the control command and drives the reflector to rotate within a small angle range by controlling the extension and retraction of the two control axes. When rotating, the tilt angle of the reflector (21) changes, causing the reflection direction of the incident light to shift, so that the image point moves between different areas on the multi-bandpass star-viewing window. The two-dimensional fast reflector (2) scans a wide area, and the star measuring component (1) collects frame-by-frame images during the acquisition and outputs them to the outside through the control circuit board (3). The outside stitches the frame-by-frame images into a large field of view image. The stitching logic is as follows: the two-dimensional fast reflector (2) has a stable scanning speed. Based on the total number of frames of the acquired images, it reverses the position of each frame image in the large field of view image, and performs image synthesis by averaging the gray values ​​of the resulting overlapping parts.

2. The hybrid star sensor daytime star measurement device as described in claim 1, characterized in that, The surface of the housing (4) is treated with black oxidation, and the inner surface through which the light path passes is sprayed with matte paint.

3. The hybrid star sensor daytime star measurement device as described in claim 1, characterized in that, The telephoto lens is designed with a large F-number.

4. The hybrid star sensor daytime star measurement device as described in claim 1, characterized in that, The two control axes (22) of the two-dimensional fast reflector (2) are not set on the same diameter of the reflector (21).

5. The hybrid star sensor daytime star measurement device as described in claim 1, characterized in that, The multi-bandpass observatory window is composed of multiple filters spliced ​​together. Each filter is a square lens and is coated with a filter film that allows the corresponding working wavelength to pass through while cutting off other wavelengths.

6. The hybrid star sensor daytime star measurement device as described in claim 1, characterized in that, The multi-bandpass star-gazing window is a square lens with different working bandpass filter films coated on different areas of its surface.

7. The hybrid star sensor daytime star measurement device as described in claim 1, characterized in that, The measurement process of the device during the day for measuring a single star is as follows: The star sensor controls the rotation of a two-dimensional fast reflector via a control circuit board to capture the star image; after the star enters the field of view, the star measurement component completes the acquisition of the star's optical image. Specifically, based on the comparison between the grayscale of the real-time acquired image and a preset threshold, it is determined whether the star's projected light passes through a suitable multi-bandpass observation window. If it is not suitable, the star sensor controls the two-dimensional fast reflector to rotate slightly via the control circuit board, changes to another position, and judges again until the grayscale of the real-time acquired image meets the requirements. The acquired clear and easily judged image is then transmitted externally after simple noise reduction and optical correction for analysis and calculation.

8. The hybrid star sensor daytime star measurement device as described in claim 1, characterized in that, When the device performs multi-star synchronous acquisition during the day, the working process is as follows: The star sensor controls the two-dimensional fast reflector to rotate rapidly through the control circuit board, sweeping across a large field of view in a short time. The frame-by-frame images acquired during this period are output and stitched together by external processing to form a large field of view image. The stitching process is as follows: the position of each frame image in the large field of view image is deduced from the total number of frames acquired. The overlapping parts are then image synthesized by averaging the gray values ​​to complete the star search and tracking within the large field of view.

Images