A solar rapid observation system and method

Abstract

This invention belongs to the field of optical system technology and discloses a rapid solar observation system and method. The invention utilizes a telescope system to collect solar light across its entire field of view; it uses a Fourier transform infrared spectrometer to acquire the solar mid- and far-infrared spectrum; it uses an imaging mirror to converge and image the coherent light emitted after the Fourier transform infrared spectrometer, obtaining primary area array imaging information at the primary image plane. This primary area array imaging information includes data in three dimensions: spatial height, spatial width, and spectral wavelength. A segmentation unit is used to segment the image spots on the primary image plane along the spatial width dimension, resulting in segmented image spots arranged sequentially in the spatial height dimension. At the secondary image plane, a linear array detector is used to acquire secondary linear array imaging information, which includes data in two dimensions: spatial height and spectral wavelength. This invention can meet the dynamic observation needs of rapidly changing solar magnetic fields.

Description

Technical Field

[0001] This invention belongs to the field of optical system technology, and more specifically, relates to a rapid solar observation system and method. Background Technology

[0002] As the central celestial body of the solar system, the Sun's radiation characteristics, atmospheric activity, and chemical composition directly influence Earth's space environment and life systems. Fourier Transform Infrared Spectrometers (FTIR), with their high resolution, wide spectral coverage, and high sensitivity, have become indispensable core equipment in the field of solar observation. By monitoring changes in solar activity's infrared radiation and utilizing the Zeeman effect in the mid-to-far-infrared band (such as the 12.32 μm MgI line), FTIR transforms solar magnetic field measurements from model-dependent "indirect measurements" to "direct measurements," potentially improving the accuracy of vector magnetic field measurements by an order of magnitude. This provides crucial support for understanding solar activity mechanisms and early warning of space weather. However, FTIR relies on the principle of interferometry to acquire the curve of detector signal intensity versus optical path difference (OPD), i.e., the interferometric signal. The desired spectral signal is obtained by performing a Fourier transform on the interferometric signal. Therefore, for each acquisition of spectral data, the moving mirror in the interferometer must complete a linear motion covering the entire OPD range, known as a spectral scan. To obtain the required high spectral resolution, long optical path difference scanning is necessary, which results in a long time for a single spectral scan. The temporal resolution (frame rate) is inversely proportional to the spectral resolution. When observing the entire sun, it would take a very long time to collect the full field of view spectrum of the sun by scanning point by point, which cannot meet the dynamic observation needs of the rapid changes in the solar magnetic field (such as flares and jets).

[0003] Currently, the mainstream imaging methods include area array imaging and linear array imaging. Area array imaging uses a two-dimensional array of detectors, which can capture a complete two-dimensional image of the target scene in a single exposure, achieving one-time imaging of a large field of view. The image information is intuitive and complete. The disadvantage is that the number of pixels per row is generally less than that of a linear array, while the total number of pixels is greater, resulting in a longer readout time and a limited frame rate, which is usually lower. This makes it difficult to meet the requirements for fine temporal resolution of rapidly changing solar processes. In actual observation, it is impossible to record the details of spectral dynamic changes caused by rapid changes in the solar magnetic field in a timely and complete manner, which is prone to motion blur or information omission, seriously affecting the in-depth research and understanding of solar physical phenomena. In contrast, linear array imaging uses a one-dimensional linear array of detectors. Through the relative motion between the detector and the target, the target is scanned row by row in a "push-broom" manner and stitched together to form a complete two-dimensional image. Thanks to its simple pixel structure and efficient readout mechanism, linear array imaging can achieve a large number of one-dimensional pixels while having a smaller total number of pixels than area array detectors. This results in extremely high data acquisition speeds, with frame rates typically two orders of magnitude higher than area array detectors, reaching 5,000 to 60,000 lines per second. This combination of fast readout and high frame rate allows for line-by-line scanning of the solar spectrum at higher frequencies, significantly enhancing the ability to monitor real-time solar changes and potentially acquiring more comprehensive and accurate solar spectral data, providing strong data support for solar physics research. However, its "pushbroom" line-by-line scanning imaging method relies on relative motion, requiring precise and stable motion control mechanisms and subsequent image stitching, a complex process that increases system complexity and cost. More importantly, for each line scanned by the linear array detector, the Fourier transform infrared spectrometer needs to perform a time-consuming spectral measurement, diminishing the advantages of fast readout and high frame rate. Summary of the Invention

[0004] This invention provides a rapid solar observation system and method, which solves the problem that existing technologies cannot meet the dynamic observation requirements of rapid changes in the solar magnetic field.

[0005] This invention provides a rapid solar observation system, comprising a telescope system, a Fourier transform infrared spectrometer, an imaging mirror, a segmentation unit, and a linear array detector arranged sequentially along the optical path. Solar full-field light is collected by the telescope system and then enters the Fourier transform infrared spectrometer, which acquires the solar mid- and far-infrared spectrum. The coherent light emitted from the Fourier transform infrared spectrometer is incident on the imaging mirror, and after being converged and imaged by the imaging mirror, primary area array imaging information is obtained at the primary image plane. This primary area array imaging information includes data in three dimensions: spatial height, spatial width, and spectral wavelength. The segmentation unit segments the image spots on the primary image plane along the spatial width dimension, and the resulting segmented image spots are arranged sequentially in the spatial height dimension. Secondary linear array imaging information is acquired at the secondary image plane using the linear array detector, and this secondary linear array imaging information includes data in two dimensions: spatial height and spectral wavelength.

[0006] Preferably, the segmentation unit is a multi-level cascaded segmentation unit composed of multiple segmentation components arranged sequentially along the optical path; the segmentation component as a first level includes an image segmentation device and a convergence component; the image segmentation device is used to segment the image spot and compensate for the optical path difference to obtain a linear image spot array of the confocal surface; the convergence component is used to converge the linear image spot array.

[0007] Preferably, the image segmentation device includes an image segmenter and a compensator arranged sequentially along the optical path; the image segmenter is used to segment the incident image spot to obtain a linear image spot array composed of multiple linear image spots arranged in a one-dimensional direction; the compensator is used to compensate for the optical path difference caused by the optical path structure of the image segmenter, so that multiple linear image spots converge on the same focal plane.

[0008] Preferably, the image segmenter includes a blade-shaped reflector and a plane reflector; the blade-shaped reflector is a plane reflector with a blade edge, the blade being used to segment image spots; the blade-shaped reflector and the plane reflector are arranged in parallel and form an optical reflection cavity; the compensator is a stepped compensator;

[0009] The knife-edge reflector is used to split the incident beam into a transmitted beam and a reflected beam;

[0010] The planar reflector is used to reflect the first reflected beam obtained after being cut by the knife-edge reflector back to the knife-edge reflector, and to emit the second reflected beam obtained after being cut by the knife-edge reflector from above or below the knife-edge reflector; wherein, the second reflected beam is the reflected beam obtained after being cut by the knife-edge reflector for the last time, and the first reflected beam is any other reflected beam besides the second reflected beam;

[0011] The stepped compensator is used to compensate for the optical path difference between the second transmitted beam and the second reflected beam. The beam after passing through the stepped compensator and the first transmitted beam together form the outgoing beam. The first transmitted beam is the transmitted beam obtained by the first splitting by the knife-edge reflector, and the second transmitted beam is any other transmitted beam besides the first transmitted beam.

[0012] Preferably, the stepped compensator is made of a light-transmitting optical material and includes multiple stepped structures, each with a different length.

[0013] Preferably, the blade angle of the blade reflector is determined by the number of segmented images.

[0014] Preferably, the converging component is a refractive or reflective type.

[0015] Preferably, the refractive converging component employs a single lens or a combination of achromatic lenses.

[0016] Preferably, the Fourier transform infrared spectrometer includes a front mirror group, a beam splitter, a fixed mirror, and a moving mirror; the front mirror group is used to collimate the incident light, and the collimated parallel light is incident on the beam splitter; the beam splitter is used to split the incident beam into a transmitted beam and a reflected beam, the reflected beam reaches the fixed mirror, and the transmitted beam reaches the moving mirror. Both the fixed mirror and the moving mirror are plane mirrors. The reflected beam and the transmitted beam return along the original path, and after being split again by the beam splitter, they form a coherent beam and are emitted.

[0017] On the other hand, the present invention provides a method for rapid solar observation, which is implemented using the aforementioned rapid solar observation system. The rapid solar observation method includes the following steps:

[0018] The entire field of view of sunlight is collected using a telescope system;

[0019] The far-infrared spectrum of the sun was obtained using a Fourier transform infrared spectrometer;

[0020] The coherent light emitted after passing through the Fourier transform infrared spectrometer is converged and imaged using an imaging mirror to obtain primary area array imaging information at the primary image plane. The primary area array imaging information includes data in three dimensions: spatial height, spatial width, and spectral wavelength.

[0021] The image spot of the primary image plane is divided along the spatial width dimension using the segmentation unit, and the resulting segmented image spots are arranged in order in the spatial height dimension;

[0022] Secondary linear array imaging information is acquired at the secondary image plane using a linear array detector. The secondary linear array imaging information includes data in two dimensions: spatial height and spectral wavelength.

[0023] One or more technical solutions provided in this invention have at least the following technical effects or advantages:

[0024] The proposed rapid solar observation scheme first uses a telescope system to collect solar light across the entire field of view. Then, it uses a Fourier transform infrared spectrometer to acquire the solar mid- and far-infrared spectrum. An imaging mirror then converges the coherent light emitted after passing through the Fourier transform infrared spectrometer to obtain primary image information at the primary image plane. This primary image information includes data in three dimensions: spatial height, spatial width, and spectral wavelength. The primary image plane is then segmented along the spatial width dimension using a segmentation unit, and the resulting segmented images are arranged sequentially in the spatial height dimension. Finally, a secondary linear array detector is used at the secondary image plane to acquire secondary linear array image information, which includes data in two dimensions: spatial height and spectral wavelength. This invention proposes a high-precision, high-spatial-resolution rapid solar observation scheme based on an image segmentation device and a Fourier transform infrared spectrometer. The invention utilizes a segmentation unit to convert area array imaging into linear array imaging via secondary imaging. This retains the high frame rate and high readout speed of linear array imaging while incorporating the advantage of area array imaging, which allows for the acquisition of full-field solar spectral data with a single spectrometer scan. It overcomes the shortcomings of low frame rate in area array imaging and the reliance on "push-broom" line-by-line scanning in linear array imaging. This breakthrough overcomes the bottleneck of low frame rate in traditional area array Fourier transform infrared spectrometers for solar observation applications, enabling direct, high-precision, and high-frame-rate measurement of high-resolution solar infrared spectra in the mid- and far-infrared bands. Attached Figure Description

[0025] Figure 1 This is a schematic diagram of the framework of a rapid solar observation system provided in Embodiment 1 of the present invention;

[0026] Figure 2 This is a schematic diagram of the image segmentation device in a rapid solar observation system provided in Embodiment 1 of the present invention;

[0027] Figure 3 This is a schematic diagram of the image plane and image spots obtained after image segmentation by the image segmentation device in a solar rapid observation system provided in Embodiment 1 of the present invention;

[0028] Figure 4 This is a schematic diagram illustrating the data format of a rapid solar observation system provided in Embodiment 1 of the present invention, which converts a primary area array image into a secondary line array image.

[0029] Among them, 1-telescope system, 2-Fourier transform infrared spectrometer, 3-imaging mirror, 4-segmentation unit, 5-linear array detector;

[0030] 210-Front lens group, 220-Beam splitter, 230-Fixed lens, 240-Moving lens;

[0031] 410 - First image segmentation device; 420 - First convergence assembly; 430 - Second image segmentation device; 440 - Second convergence assembly;

[0032] 411-Knife-edge reflector, 412-Plane reflector, 413-Stepped compensator. Detailed Implementation

[0033] To better understand the above technical solutions, the following will provide a detailed explanation of the technical solutions in conjunction with the accompanying drawings and specific implementation methods.

[0034] Example 1:

[0035] Example 1 provides a rapid solar observation system, see [link to example]. Figure 1 and Figure 4 The system comprises a telescope system 1, a Fourier transform infrared spectrometer 2, an imaging mirror 3, a segmentation unit 4, and a linear array detector 5, arranged sequentially along the optical path. Solar full-field-of-view light is collected by the telescope system 1 and then enters the Fourier transform infrared spectrometer 2, which acquires the solar mid- and far-infrared spectrum. The coherent light emitted from the Fourier transform infrared spectrometer 2 is incident on the imaging mirror 3, and after being converged and imaged by the imaging mirror 3, primary area array imaging information is obtained at the primary image plane. This primary area array imaging information includes data in three dimensions: spatial height, spatial width, and spectral wavelength. The segmentation unit 4 segments the image spots of the primary image plane along the spatial width dimension, and the resulting segmented image spots are arranged sequentially in the spatial height dimension. Secondary linear array imaging information is acquired at the secondary image plane using the linear array detector 5, and this secondary linear array imaging information includes data in two dimensions: spatial height and spectral wavelength.

[0036] The main function of the telescope system 1 is to collect sunlight using a primary mirror (reflective) or an objective lens (refractive) and focus the light onto the focal plane to form a real image of the sun, which facilitates further processing and analysis.

[0037] Among them, the Fourier transform infrared spectrometer 2 is a key device for acquiring solar mid- and far-infrared spectral signals. It uses an interferometer to measure the interference signal of infrared light, and then converts the time-domain signal into a frequency-domain spectrum through Fourier transform mathematical processing. Based on the Zeeman effect of mid- and far-infrared spectral lines (such as the 12.32 μm MgI spectral line), it realizes the direct measurement of the solar magnetic field.

[0038] For example, see Figure 1The Fourier transform infrared spectrometer 2 includes a front mirror group 210, a beam splitter 220, a fixed mirror 230, and a moving mirror 240. The front mirror group 210 is used to collimate the incident light, and the collimated parallel light is incident on the beam splitter 220. The beam splitter 220 is used to split the incident beam into a transmitted beam and a reflected beam. The reflected beam reaches the fixed mirror 230, and the transmitted beam reaches the moving mirror 240. Both the fixed mirror 230 and the moving mirror 240 are plane mirrors. The reflected beam and the transmitted beam return along the original path and are split again by the beam splitter 220 to form a coherent beam and then emitted.

[0039] The imaging mirror 3 is used to focus the light that has been modulated by the Fourier transform infrared spectrometer 2 to form an image.

[0040] The main function of the segmentation unit 4 is to segment the area array image spots of the single imaging after scanning by the Fourier transform infrared spectrometer 2 into vertically arranged linear array image spots, thereby realizing the conversion of area array image spots into linear array image spots. This efficiently utilizes the high readout speed and high frame rate of linear array imaging, while making up for the shortcomings of linear array imaging, which requires precise motion control and multiple long-time spectral scans. This improves the frame rate of solar full-field spectral imaging detection, so as to cope with the scenario of rapid changes in solar surface activity and magnetic field, and further improves the real-time performance of solar observation.

[0041] Specifically, the segmentation unit 4 is a multi-level cascaded segmentation unit composed of multiple segmentation components arranged sequentially along the optical path; the segmentation component as a first level includes an image segmentation device and a convergence component; the image segmentation device is used to segment the image spot and compensate for the optical path difference to obtain a linear image spot array of the confocal surface; the convergence component is used to converge the linear image spot array.

[0042] For example, see Figure 1 The segmentation unit 4 is a two-stage cascaded segmentation unit, including a first image segmentation device 410, a first convergence component 420, a second image segmentation device 430, and a second convergence component 440 arranged sequentially along the optical path; wherein, the first image segmentation device 410 and the first convergence component 420 constitute a first-stage segmentation component, and the second image segmentation device 430 and the second convergence component 440 constitute a second-stage segmentation component.

[0043] The converging components (e.g., the first converging component 420 and the second converging component 440) are refractive or reflective; the refractive converging components can be single lenses or combinations of achromatic lenses. The optical parameters of the converging components can be determined according to the image plane size of the linear array detector 5.

[0044] The image segmentation device includes an image segmenter and a compensator arranged sequentially along the optical path; the image segmenter is used to segment the incident image spot to obtain a linear image spot array composed of multiple linear image spots arranged in a one-dimensional direction; the compensator is used to compensate for the optical path difference caused by the optical path structure of the image segmenter, so that multiple linear image spots converge on the same focal plane.

[0045] See Figure 2 The image segmenter includes a blade-shaped reflector 411 and a plane reflector 412; the blade-shaped reflector 411 is a plane reflector with a blade edge, and the blade edge is used to segment the image spot; the blade-shaped reflector 411 and the plane reflector 412 are arranged in parallel and form an optical reflection cavity; the compensator adopts a stepped compensator 413.

[0046] The incident light beam enters the optical reflection cavity, and the knife-edge reflector 411 is used to split the incident light beam into a transmitted beam and a reflected beam.

[0047] The planar reflector 412 is used to reflect the first reflected beam obtained after being cut by the knife-edge reflector 411 back to the knife-edge reflector 411, and to emit the second reflected beam obtained after being cut by the knife-edge reflector 411 from above or below the knife-edge reflector 411; wherein, the second reflected beam is the reflected beam obtained after being cut by the knife-edge reflector 411 for the last time, and the first reflected beam is any other reflected beam besides the second reflected beam.

[0048] The stepped compensator 413 is used to compensate for the optical path difference between the second transmitted beam and the second reflected beam. The beam after passing through the stepped compensator 413 and the first transmitted beam together form the outgoing beam. The first transmitted beam is the transmitted beam obtained by the first split by the knife-edge reflector 411, and the second transmitted beam is other transmitted beams besides the first transmitted beam.

[0049] That is, the knife-edge reflector 411 is a plane reflector with a knife-edge, its edge being sharp and burr-free, capable of slicing the image spot. The upper or lower edge of the knife-edge reflector 411 should ensure that the second reflected beam can be emitted completely without being sliced ​​(e.g., Figure 2 The upper edge of the knife-edge reflector 411 ensures that the second reflected beam can exit completely without being split. The plane reflector 412 ensures that the incident beam enters the optical reflection cavity completely, and all reflected light after being reflected by the knife-edge reflector 411 can be completely reflected by the plane reflector 412.

[0050] Since the segmented image spots are generated by repeated incident of circular light spots onto the optical edge of the blade-shaped reflector 411, different image spots will have different optical path lengths when reaching the optical edge. This results in different imaging positions of different segmented images along the optical axis, leading to defocusing and blurring of the segmented image spots. This invention utilizes the stepped compensator 413 to compensate for the different optical path differences generated by the optical reflection cavity, thereby solving the problem of blurred segmented image spots. The stepped compensator 413 is specifically made of a light-transmitting optical material and includes multiple stepped structures, each with a different length.

[0051] See Figure 2 The incident beam is incident on the knife-edge reflector 411 at an incident angle of θ. To reduce the defocusing amount, the incident angle θ can be appropriately increased, while the thickness of the reflective cavity can be minimized. However, increasing the incident angle will cause more object points to be segmented into different segmented images, making the object point repetition more serious. To ensure the imaging quality, θ = 45° is set. At this time, the optical path corresponding to the unit image spot diameter is the smallest, the image spot diffusion degree is the smallest, and the system transmittance is the largest.

[0052] The distance between the knife-edge reflector 411 and the plane reflector 412 is the thickness of the optical reflection cavity. The thickness of the optical reflection cavity can be determined based on the image spot diameter of the front optical system, the focal ratio of the incident beam, and the incident angle θ.

[0053] The image segmenter is positioned on the optical axis of the incident beam. The Fourier transform infrared spectrometer 2 images near the optical segmentation edge of the knife-edge reflector 411. Each time the incident beam passes through the knife-edge reflector 411, it is split into two beams. One beam is transmitted through the knife edge to obtain a segmented image, and the other beam is reflected back to the plane reflector 412. Through multiple transmissions and reflections by the knife-edge reflector 411 and the plane reflector 412, multiple segmented images can be separated. This process is repeated to complete the image segmentation. The distribution of the segmented image spots is as follows: Figure 3 As shown.

[0054] The blade angle of the blade-shaped reflector 411 is determined by the number of segmented images. For details, see [link to documentation]. Figure 3 , The blade angle of the blade reflector 411 is such that, to ensure that the diameter of the light spot remains constant each time it reaches the optical blade during the slicing process, the blade angle of the blade reflector 411 needs to be determined based on the number of slicing images. Specifically, it can be calculated using the following formula: In the formula, n is the number of segmented images.

[0055] The incident beam's initial bisector position on the optical blade of the blade-shaped reflector 411 determines the final shape of the bisector image. Based on experimental comparisons, it was found that four bisector images produce better imaging results. Therefore, the preferred bisector position is one where the final bisector image is a four-part linear image with equal width. Figure 3 As shown. Furthermore, the number of reflections within the optical cavity and the number of steps in the stepped compensator 413 can be changed according to actual needs. The image segmentation device can also be designed to rotate along the optical axis or by adding additional rearrangement components to make the final image a vertical array.

[0056] The following example uses a four-part linear image spot, corresponding to a stepped compensator 413 with three stepped layers, as an example. Figure 2 Let's illustrate with examples.

[0057] See Figure 2 An incident light beam enters the reflecting cavity formed by the knife-edge reflector 411 and the plane reflector 412. The incident light beam is then split into two beams by the knife-edge of the knife-edge reflector 411, denoted as the transmitted beam t1 and the reflected beam r1, respectively. The reflected beam r1 is reflected by the plane reflector 412 and then returns to the knife-edge reflector 411, where it is further split into two beams, denoted as the transmitted beam t2 and the reflected beam r2, respectively. The reflected beam r2 is also reflected by the plane reflector 412 and then returns to the knife-edge reflector 411. The blade-edge reflector 411 then divides the light beam into two beams, denoted as transmitted beam t3 and reflected beam r3, respectively. Reflected beam r3 is reflected by the plane reflector 412 and exits from above the blade-edge reflector 411. Transmitted beam t2, transmitted beam t3, and reflected beam r3 then enter the stepped compensator 413, passing sequentially through the bottom, middle, and top layers. After exiting, they combine with the transmitted beam t1 to form the divided outgoing beam, completing the conversion from surface light to line light. Since different segmented image spots are generated by multiple reflections of circular image spots through the optical reflection cavity and then through the optical blade, the optical path lengths of different image spots reaching the optical edge are different. The more reflections, the longer the optical path, resulting in different imaging positions of different segmented images along the optical axis, causing defocusing and blurring of the segmented image spots. Therefore, it is necessary to add the stepped compensator 413 to the exit paths of the transmitted beam t2, the transmitted beam t3, and the reflected beam r3 to compensate for the different optical path differences generated by them passing through the optical reflection cavity, so as to alleviate the defocusing phenomenon of the image spot and ensure the imaging quality. Figure 3 The black area represents light passing through the blade-shaped reflector 411, and the white area represents light reflected back to the plane reflector 412 by the blade-shaped reflector 411.

[0058] Considering that the ability of the stepped compensator 413 to compensate for the optical path of the outgoing light is limited, the number of layers of the stepped compensator 413 should not be too many. Therefore, this invention preferably divides the incident beam into four equal segments. If the number of segments is too large, defocusing will be difficult to compensate for; while reducing the number of segmented images will increase the width of a single segmented image, making it difficult for the linear array detector to capture the entire width of the segmented image at once. To better compensate for defocusing while increasing the number of segmented images and obtaining sufficiently narrow segmented images, enabling the linear array detector to capture the entire field of view image spot at once, this invention cascades multiple image segmentation devices with a converging component, for example... Figure 1 The two-stage cascaded configuration shown has the image segmenter device (i.e., the second image segmentation device 430) placed in front of the imaging image of the converging component (i.e., the first converging component 420) of the previous stage. The second converging component 440 is used to converge the second-stage segmented image. Each stage segmentation component only segments a small number of image spots. Through multi-stage cascading, the defocus phenomenon is better compensated, while increasing the number of segmented image spots and reducing the width of the segmented image spots. This can meet the requirement of linear array detectors to acquire full-field target image spots at one time, greatly reducing the number of spectral scans and improving the efficiency of solar full-field infrared spectrum acquisition and magnetic field observation.

[0059] The linear array detector 5 is located at the output end of the segmentation unit 4. It is used to receive one-dimensional linear array images and read out data at a high frame rate, thereby achieving high-speed acquisition of solar full-field spectral information. For example, the linear array detector 5 can be an infrared linear array detector with global shutter mode.

[0060] Figure 4 This is a data illustration corresponding to the present invention, including primary area array imaging data and secondary linear array imaging data after conversion to an array form. The primary imaging area array data is three-dimensional data at the primary image plane after passing through the Fourier transform infrared spectrometer 2, including three dimensions: spatial height H, spatial width W, and spectral wavelength λ, which together form an "imaging spectral cube". After image spot segmentation by the segmentation unit 4, the image spots of the primary image plane are segmented along the spatial width W dimension. The segmented image spots are arranged sequentially along the spatial height H dimension. Secondary imaging linear array data can be acquired at the secondary image plane using the linear array detector 5. Unlike the primary area array imaging data, the secondary linear array imaging data includes two dimensions: spatial height H and spectral wavelength λ. The image segmentation group only affects the spatial dimension information of the data. The spectral dimension information is generated by the displacement of the moving mirror 240 in the Fourier transform infrared spectrometer 2.

[0061] Overall, the target solar full-field light, after being collected by the telescope system 1, enters the Fourier transform infrared spectrometer 2. Utilizing the displacement of the moving mirror 240 within the Fourier transform infrared spectrometer 2, an optical path difference is created between the two coherent beams reflected by the moving mirror 240 and the fixed mirror 230, resulting in interference at the image plane. The infrared interference signal is measured, and a Fourier transform is performed on the interference signal to obtain the mid-to-far-infrared spectrum containing information such as the solar magnetic field. The light after passing through the Fourier transform infrared spectrometer 2 is then converged by the imaging mirror 3 to obtain area array imaging data at the primary image plane. By adding the segmentation unit 4 before the primary image plane, the two-dimensional image spot of the sun at the primary image plane can be segmented into multiple longitudinally arranged sub-images through the combination of the knife-edge reflector 411, the plane reflector 412, and the stepped compensator 413, thus completing the transformation from a planar array to a linear array. The linear array detector 5 can obtain the required three-dimensional "imaging spectral cube" data of the sun's full field of view in one go. This not only retains the advantages of the high readout speed and high frame rate of the linear array detector, but also omits the "push-broom" line-by-line imaging step required for linear array imaging, reducing the number of spectral scans and further improving the efficiency of linear array imaging. It can achieve high frame rate detection of solar mid- and far-infrared spectral and magnetic field information, further improving the efficiency of solar observation.

[0062] The solar rapid observation system provided in Example 1 can acquire solar full-field "spectral cube" data using the Fourier transform infrared spectrometer 2. It achieves solar magnetic field measurement based on the Zeeman effect of mid- and far-infrared spectral lines (such as the 12.32 μm MgI line). Simultaneously, utilizing the area-to-linear array imaging technology of the segmentation unit 4, it eliminates the cumbersome "push-broom" line-by-line imaging steps of linear array imaging. Only one spectral scan is needed to obtain the spectral data of all pixels in the target's full field of view, further improving the accuracy and real-time performance of solar infrared spectral and magnetic field observations. In other words, to overcome the shortcomings of both area array imaging and linear array imaging and leverage their respective advantages, this invention adopts a technical approach that combines area array imaging and linear array imaging. The area array is converted to a linear array using an image segmentation device and then re-imaged onto the image plane of the linear array detector 5. Furthermore, considering that traditional image segmentation devices, such as the most widely used Bowen-Walraven image segmenter (BW image segmenter), introduce problems such as image defocusing and blurred edge spots during the conversion from area array to linear array, this invention also compensates for the optical path difference introduced by the image segmenter that causes defocusing of linear spots by adding a compensator, which can further improve the imaging quality.

[0063] Based on the above description, the solar rapid observation system provided in Example 1 has the following advantages:

[0064] (1) High-speed imaging. Area array imaging requires simultaneous exposure of the entire two-dimensional array of detectors, resulting in a long readout time and limited frame rate, which easily leads to motion blur when photographing high-speed moving targets. While traditional linear array imaging has a faster scanning speed, it is limited by the relative motion control precision and requires "push-broom" line-by-line imaging. The spectrometer needs to perform spectral data acquisition once for each line of imaging, which limits the overall efficiency. This invention converts a single area array imaging into a secondary linear array imaging in real time through an image segmenter, reducing the time cost of repeated exposure and spectral scanning for line-by-line imaging. The optical conversion response speed of the image segmenter system is much higher than that of mechanical motion control, which can quickly convert area array information into linear array output. Combined with the high-speed data acquisition capability of the detector, the imaging frame rate of the system is greatly improved, enabling clear and rapid capture of the dynamic process of high-speed changing solar surface activity.

[0065] (2) Large field-of-view imaging. Traditional linear array imaging is limited to the field of view of a single linear array, requiring complex motion stitching to cover a large range of targets, a cumbersome process prone to stitching errors; while area array imaging has a larger field of view, it is difficult to maintain spatial resolution. This invention combines the advantages of the large field of view of area array imaging with the high-resolution characteristics of linear array imaging: the initial area array imaging can acquire information about a large range of targets at once, and the image segmenter system retains the field of view of the original area array during the conversion process, achieving mode conversion only through optical segmentation, without relying on mechanical motion to expand the field of view. Therefore, the system naturally possesses the capability of large field of view imaging, without the need for complex mechanical motion control and image stitching algorithms, avoiding the field of view stitching errors and system complexity caused by these, and ensuring the integrity and consistency of the observation data.

[0066] (3) Simple structure and easy miniaturization. The present invention uses the image segmenter as the core optical element, which can adopt an integrated prism or microlens array structure, eliminating the need for mechanical moving parts. It adopts a common reference assembly method with the detector image plane. By optimizing the optical path design and eliminating redundant components, the overall volume and weight are significantly reduced, which can meet the stringent requirements of various platforms for equipment miniaturization and lightweighting. At the same time, the simplified structure effectively reduces the assembly complexity and potential failure risk, which is more conducive to achieving lightweight and compact integration of the system.

[0067] (4) Low cost and easy to promote. The use of mature and relatively low-cost high-performance linear array detectors replaces the expensive high-speed area array detectors, which greatly reduces the cost and development risk of the detector subsystem. At the same time, it avoids the need for precision mechanical movement in traditional linear array "push-broom" imaging, which not only reduces hardware manufacturing costs, but also reduces the system debugging, calibration and long-term operation maintenance costs.

[0068] In summary, this invention achieves breakthroughs in imaging rate, field-of-view structure compactness, and cost through optical design innovation and system optimization, providing an efficient and reliable technical solution for realizing rapid solar observation.

[0069] Example 2:

[0070] Example 2 provides a method for rapid solar observation, implemented using the rapid solar observation system described in Example 1. The rapid solar observation method includes the following steps:

[0071] The entire field of view of sunlight is collected using a telescope system;

[0072] The far-infrared spectrum of the sun was obtained using a Fourier transform infrared spectrometer;

[0073] The coherent light emitted after passing through the Fourier transform infrared spectrometer is converged and imaged using an imaging mirror to obtain primary area array imaging information at the primary image plane. The primary area array imaging information includes data in three dimensions: spatial height, spatial width, and spectral wavelength.

[0074] The image spot of the primary image plane is divided along the spatial width dimension using the segmentation unit, and the resulting segmented image spots are arranged in order in the spatial height dimension;

[0075] Secondary linear array imaging information is acquired at the secondary image plane using a linear array detector. The secondary linear array imaging information includes data in two dimensions: spatial height and spectral wavelength.

[0076] That is, the present invention first uses a telescope system and a Fourier transform infrared spectrometer to perform a complete spectral scan of the solar full field of view, generating interferogram data containing spatial and spectral information of the entire field of view, and forming a two-dimensional array image spot on a single image plane; then, the two-dimensional array image spot is segmented and rearranged into a one-dimensional linear array image spot in real time using a segmentation unit; finally, all the data of the one-dimensional linear array image spot is read out at once using a linear array detector, completing the acquisition of three-dimensional "imaging spectral cube" data of the solar full field of view.

[0077] The acquired data can then be subjected to Fourier transform to obtain the infrared spectra at various spatial locations. Furthermore, by analyzing the Zeeman effect of characteristic spectral lines in the mid- and far-infrared bands (such as the MgI 12.32 μm line), the distribution of the solar magnetic field can be retrieved. It should be noted that the core improvement of this invention lies in the rapid acquisition of solar "imaging spectral cube" data; subsequent data processing and analysis can be implemented based on existing research.

[0078] Since the observation method provided in Example 2 corresponds to the function of each device in the observation system provided in Example 1, Example 2 can be understood by referring to the description of Example 1, and will not be repeated here.

[0079] In summary, this invention solves the dual bottlenecks of low frame rate in existing area array imaging Fourier transform infrared spectrometers for mid- and far-infrared solar observations and low efficiency of traditional linear array imaging's "push-broom" line-by-line scanning. This invention utilizes a Fourier transform infrared spectrometer to acquire interferogram data of the entire solar field of view. Then, through a cascaded image segmentation device located at the primary image plane, the two-dimensional area array image spots are segmented and rearranged into one-dimensional linear array image spots in real time and efficiently, and finally read out by a high-frame-rate linear array detector. This invention cleverly combines the advantages of area array imaging's "single-scan acquisition of the entire field of view spectrum" and the advantages of linear array detectors' "high-speed readout." By using pure optical conversion, it avoids the mechanical "push-broom" line-by-line imaging process of linear array imaging, significantly improving the system's effective observation frame rate and real-time performance, and achieving high-precision, high-spatial-resolution rapid detection of solar mid- and far-infrared spectral and magnetic field information.

[0080] Finally, it should be noted that the above specific embodiments are only used to illustrate the technical solutions of the present invention and not to limit it. Although the present invention has been described in detail with reference to examples, those skilled in the art should understand that modifications or equivalent substitutions can be made to the technical solutions of the present invention without departing from the spirit and scope of the technical solutions of the present invention, and all such modifications or substitutions should be covered within the scope of the claims of the present invention.

Claims

1. A rapid solar observation system, characterized in that, The system comprises a telescope system, a Fourier transform infrared spectrometer, an imaging mirror, a segmentation unit, and a linear array detector, arranged sequentially along the optical path. Solar full-field light is collected by the telescope system and then enters the Fourier transform infrared spectrometer, which acquires the solar mid- and far-infrared spectrum. The coherent light emitted from the Fourier transform infrared spectrometer is incident on the imaging mirror, and after being converged and imaged by the imaging mirror, primary area array imaging information is obtained at the primary image plane. This primary area array imaging information includes data in three dimensions: spatial height, spatial width, and spectral wavelength. The segmentation unit segments the image spots on the primary image plane along the spatial width dimension, and the resulting segmented image spots are arranged sequentially in the spatial height dimension. Secondary linear array imaging information is acquired at the secondary image plane using the linear array detector, and this secondary linear array imaging information includes data in two dimensions: spatial height and spectral wavelength. The segmentation unit is a multi-level cascaded segmentation unit composed of multiple segmentation components arranged sequentially along the optical path; the segmentation component as a first level includes an image segmentation device and a convergence component; the image segmentation device is used to segment the image spot and compensate for the optical path difference to obtain a linear image spot array of the confocal surface; the convergence component is used to converge the linear image spot array. The Fourier transform infrared spectrometer includes a front mirror group, a beam splitter, a fixed mirror, and a moving mirror. The front mirror group is used to collimate the incident light, and the resulting parallel light is incident on the beam splitter. The beam splitter is used to split the incident beam into a transmitted beam and a reflected beam. The reflected beam reaches the fixed mirror, and the transmitted beam reaches the moving mirror. Both the fixed mirror and the moving mirror are plane mirrors. The reflected beam and the transmitted beam return along the same path and are split again by the beam splitter to form a coherent beam before being emitted.

2. The rapid solar observation system according to claim 1, characterized in that, The image segmentation device includes an image segmenter and a compensator arranged sequentially along the optical path; the image segmenter is used to segment the incident image spot to obtain a linear image spot array composed of multiple linear image spots arranged in a one-dimensional direction; the compensator is used to compensate for the optical path difference caused by the optical path structure of the image segmenter, so that multiple linear image spots converge on the same focal plane.

3. The rapid solar observation system according to claim 2, characterized in that, The image segmenter includes a blade-shaped reflector and a plane reflector; the blade-shaped reflector is a plane reflector with a blade edge, which is used to segment image spots; the blade-shaped reflector and the plane reflector are arranged in parallel and form an optical reflection cavity; the compensator is a stepped compensator. The knife-edge reflector is used to split the incident beam into a transmitted beam and a reflected beam; The planar reflector is used to reflect the first reflected beam obtained after being cut by the knife-edge reflector back to the knife-edge reflector, and to emit the second reflected beam obtained after being cut by the knife-edge reflector from above or below the knife-edge reflector; wherein, the second reflected beam is the reflected beam obtained after being cut by the knife-edge reflector for the last time, and the first reflected beam is any other reflected beam besides the second reflected beam; The stepped compensator is used to compensate for the optical path difference between the second transmitted beam and the second reflected beam. The beam after passing through the stepped compensator and the first transmitted beam together form the outgoing beam. The first transmitted beam is the transmitted beam obtained by the first splitting by the knife-edge reflector, and the second transmitted beam is any other transmitted beam besides the first transmitted beam.

4. The rapid solar observation system according to claim 3, characterized in that, The stepped compensator is made of a light-transmitting optical material and includes multiple stepped structures, each with a different length.

5. The rapid solar observation system according to claim 3, characterized in that, The blade angle of the blade reflector is determined by the number of segmented images.

6. The rapid solar observation system according to claim 1, characterized in that, The converging component is either refractive or reflective.

7. The rapid solar observation system according to claim 6, characterized in that, Refractive converging components employ either a single lens or a combination of achromatic lenses.

8. A method for rapid solar observation, characterized in that, The method of rapid solar observation, implemented using any one of claims 1 to 7, comprises the following steps: The entire field of view of sunlight is collected using a telescope system; The far-infrared spectrum of the sun was obtained using a Fourier transform infrared spectrometer; The coherent light emitted after passing through the Fourier transform infrared spectrometer is converged and imaged using an imaging mirror to obtain primary area array imaging information at the primary image plane. The primary area array imaging information includes data in three dimensions: spatial height, spatial width, and spectral wavelength. The image spot of the primary image plane is divided along the spatial width dimension using the segmentation unit, and the resulting segmented image spots are arranged in order in the spatial height dimension; Secondary linear array imaging information is acquired at the secondary image plane using a linear array detector. The secondary linear array imaging information includes data in two dimensions: spatial height and spectral wavelength.

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