A wide-energy-spectrum high-dynamic-range solar X-ray flare monitor

Abstract

This invention relates to a wide-spectrum, high dynamic range solar X-ray flare monitor, comprising an X-ray probe unit and a processing circuit unit. The X-ray probe unit receives X-rays emitted by the sun, converts the optical signal of the X-rays into an electrical signal, and sends the electrical signal to the processing circuit unit. The processing circuit unit processes the received electrical signal, converting it into X-ray information including energy and intensity, thereby achieving wide-spectrum, high dynamic range solar X-ray flare monitoring. This invention employs a dual-channel design, enabling high dynamic range detection of solar X-ray radiation flux exceeding five orders of magnitude and fine detection of solar spectral information.

Description

Technical Field

[0001] This invention relates to a wide-spectrum, high-dynamic-range solar X-ray flare monitor, belonging to the field of space X-ray detection technology. Background Technology

[0002] Solar X-ray bursts are rapid intensifications of solar X-ray radiation, classified into hard X-ray bursts (10 keV-100 MeV) and soft X-ray bursts (1-10 keV). According to international standards, a solar soft X-ray flare is defined as the peak electromagnetic flux in the 1-8A band at a distance of 1 astronomical unit from the Sun outside the Earth's atmosphere. The dynamic range of solar soft X-ray flare flux is extremely wide, classified into five levels: A, B, C, M, and X, with X being the highest. The photon flux differs by one order of magnitude between each level, and each level is further subdivided into 100 sub-levels.

[0003] Traditional solar X-ray monitors are divided into two types: soft X-ray monitors and hard X-ray monitors. Soft X-ray monitors are generally designed to observe energy ranges of 1-30 keV, using silicon-based X-ray detectors and employing a single-channel design, resulting in lower energy resolution and dynamic range. Hard X-ray monitors are generally designed to observe energy ranges of 30-700 keV, using X-ray scintillator detectors and employing a single-channel design, also resulting in lower energy resolution and poorer dynamic range. Summary of the Invention

[0004] The technical problem solved by this invention is to overcome the shortcomings of the prior art and propose a wide-spectrum, high-dynamic-range solar X-ray flare monitor. It adopts a dual-channel design and can realize high dynamic range detection of solar X-ray radiation flux intensity of more than 5 orders of magnitude and fine detection of solar spectral information.

[0005] The solution of the present invention is:

[0006] A wide-spectrum, high-dynamic-range solar X-ray flare monitor includes an X-ray probe unit and a processing circuit unit. The X-ray probe unit receives X-rays emitted by the sun, converts the optical signal of the X-rays into an electrical signal, and sends the electrical signal to the processing circuit unit. The processing circuit unit processes the received electrical signal and converts the electrical signal into X-ray information including energy and intensity, thereby realizing wide-spectrum, high-dynamic-range solar X-ray flare monitoring.

[0007] Furthermore, the X-ray probe unit includes a low-energy detection module and a high-energy detection module, both of which, along the direction of sunlight, sequentially include an aperture, a movable baffle, an observation window, and a detector.

[0008] Furthermore, there are multiple apertures, each with a light-transmitting hole that decreases in size along the direction of sunlight.

[0009] Furthermore, the angle between the light ray and the optical axis is 1°-30°.

[0010] Furthermore, a movable baffle is set on the optical axis, and a filter is set in the observation window to filter out light rays other than X-rays.

[0011] Furthermore, the low-energy detection module adopts a dual-channel design with two X-ray silicon drift detectors, and the observation window uses a beryllium filter, with the two channels having the same field of view.

[0012] Furthermore, the high-energy detection module adopts a dual-channel design with two tellurium zinc cadmium detectors and aluminum filters for the observation window, ensuring that the observation fields of both channels are identical.

[0013] Furthermore, the movable baffle is made of a two-layer structure of copper and aluminum, and is driven by a motor and can be positioned at the front end of the dual-channel detector.

[0014] Furthermore, in the normal observation mode of the low-energy detection module, the movable baffle is positioned at the front end of any X-ray silicon drift detector, so that the effective observation areas of the dual-channel detectors are of different sizes, in order to expand the dynamic observation range for solar eruption activities such as flares of different levels.

[0015] When either detector fails, the movable baffle blocks the failed detector when the sun is calm, allowing observations to be made using the normal detector; when a solar flare erupts, the movable baffle blocks the normal detector, limiting the effective observation area of ​​the normal detector. Thus, even if either detector in the dual channels fails, high dynamic range observations of solar eruption activities of different levels of flares can still be guaranteed.

[0016] Furthermore, in the normal observation mode of the high-energy detection module, the movable baffle is positioned at the front end of either cadmium zinc telluride detector, so that the detection efficiency of the dual-channel detectors is different, thereby expanding the dynamic observation range of solar eruption activities for different levels of flares, while increasing the effective observation area and improving the observation sensitivity of solar high-energy X-rays.

[0017] When either detector fails, the movable baffle blocks the failed detector when the sun is calm, allowing observations to be made using the normal detector; when a solar flare erupts, the movable baffle blocks the normal detector, limiting its detection efficiency. Thus, even if either detector in the dual channels fails, high dynamic range observations of solar eruption activity of different levels of flares can still be guaranteed.

[0018] Furthermore, the processing circuit unit includes a front-end electronics module, a digital processing circuit module, and a power board module.

[0019] The digital processing circuit module includes a signal processing unit and a processor circuit unit, while the power supply board module includes a secondary power supply unit and a high-voltage power supply unit.

[0020] The front-end electronics module amplifies and converts the detector output signal into digital data before it enters the signal processing unit. The signal processing unit implements X-ray single-photon signal processing based on FPGA. The processor circuit unit collects the detector's operating status and temperature, collects the signal processing unit's operating status and observed energy spectrum data, controls the power supply and power-on sequence of the signal processing unit, and realizes communication with the satellite platform.

[0021] The secondary power supply unit provides power to the detector, while the high-voltage power supply unit provides the high voltage required for the detector to operate.

[0022] The advantages of this invention compared to the prior art are:

[0023] (1) This invention integrates the design of a multi-channel X-ray detector, and under the constraints of limited weight and volume, realizes the monitoring of solar X-ray flares with a wide energy spectrum, high energy resolution and high dynamic range. The detection energy spectrum covers 1keV-700keV, and the energy resolution reaches 160eV@5.9keV, 8%@59.5keV and 3%@662keV. It can realize the detection of solar X-ray radiation flux intensity with a high dynamic range of more than 5 orders of magnitude.

[0024] (2) This invention innovatively adopts a dual-channel high-dynamic detection design for soft X-rays. The front end of the soft X-ray detector is designed with a movable baffle, which is made of a two-layer stacked structure of copper and aluminum. In normal observation mode, the dynamic observation range for solar eruptions such as flares of different levels can be expanded by setting different effective observation areas. In the event of an anomaly in either detector, the high-dynamic range of observation of solar eruptions such as flares of different levels can still be guaranteed by adjusting the opening and closing state of the baffle. At the same time, the two channels serve as backups for each other, enhancing the reliability of the instrument.

[0025] (3) This invention innovatively adopts a dual-channel high-dynamic detection design for hard X-rays. The front end of the dual-channel hard X-ray detector is designed with a movable baffle, which is made of a two-layer stacked structure of copper and aluminum. In normal observation mode, the dynamic observation range for solar eruptions such as flares of different levels can be expanded by setting different observation efficiencies, while increasing the effective observation area and improving the observation sensitivity of solar high-energy X-rays. In the event of an anomaly in either detector, the high-dynamic range observation of solar eruptions such as flares of different levels can still be guaranteed by adjusting the opening and closing state of the baffle. At the same time, the two channels serve as backups for each other, enhancing the reliability of the instrument. Attached Figure Description

[0026] Figure 1 This is a schematic diagram of the components of the wide-spectrum, high dynamic range solar X-ray flare monitor of the present invention;

[0027] Figure 2 This is a schematic diagram of the front end of the wide-spectrum, high dynamic range solar X-ray flare monitor of the present invention;

[0028] Figure 3This is a schematic diagram of the processing circuit principle of the wide-spectrum, high-dynamic-range solar X-ray flare monitoring instrument of the present invention. Detailed Implementation

[0029] The present invention will be further described below with reference to the embodiments.

[0030] A wide-spectrum, high dynamic range solar X-ray flare monitor, such as Figure 1-3 As shown, it includes an X-ray probe unit 1 and a processing circuit unit 2. The X-ray probe unit 1 receives X-rays emitted by the sun, converts the optical signal of the X-rays into an electrical signal, and sends the electrical signal to the processing circuit unit 2. The processing circuit unit 2 processes the received electrical signal and converts the electrical signal into X-ray information including energy and intensity, so as to realize the monitoring of solar X-ray flares with a wide energy spectrum and high dynamic range.

[0031] X-ray probe unit 1 includes a low-energy detection module and a high-energy detection module. Both modules include, in sequence along the direction of sunlight, an aperture 5, a movable baffle 6, an observation window 7, and a detector.

[0032] There are multiple apertures 5, each with a light-transmitting hole that decreases in size along the direction of sunlight.

[0033] The angle between the ray and the optical axis is 1°-30°.

[0034] A movable baffle 6 is set on the optical axis, and a filter is set in the observation window 7 to filter out light rays other than X-rays.

[0035] The low-energy detection module adopts a dual-channel design with two X-ray silicon drift detectors and a beryllium filter for the observation window, with the two channels having the same field of view.

[0036] The high-energy detection module adopts a dual-channel design with two tellurium zinc cadmium detectors and aluminum filters in the observation window, with the two channels having the same field of view.

[0037] The movable baffle is made of a two-layer structure of copper and aluminum. The movable baffle is driven by a motor and can be positioned at the front end of the dual-channel detector.

[0038] In the normal observation mode of the low-energy detection module, the movable baffle is positioned at the front end of any X-ray silicon drift detector, so that the effective observation areas of the dual-channel detectors are large and small, in order to expand the dynamic observation range for solar eruption activities such as flares of different levels.

[0039] When either detector fails, the movable baffle blocks the failed detector when the sun is calm, allowing observations to be made using the normal detector; when a solar flare erupts, the movable baffle blocks the normal detector, limiting the effective observation area of ​​the normal detector. Thus, even if either detector in the dual channels fails, high dynamic range observations of solar eruption activities of different levels of flares can still be guaranteed.

[0040] In the normal observation mode of the high-energy detection module, the movable baffle is positioned at the front end of either zinc cadmium telluride detector, so that the detection efficiency of the two-channel detectors is different, thereby expanding the dynamic observation range of solar eruption activities for different levels of flares, while increasing the effective observation area and improving the observation sensitivity of solar high-energy X-rays.

[0041] When either detector fails, the movable baffle blocks the failed detector when the sun is calm, allowing observations to be made using the normal detector; when a solar flare erupts, the movable baffle blocks the normal detector, limiting its detection efficiency. Thus, even if either detector in the dual channels fails, high dynamic range observations of solar eruption activity of different levels of flares can still be guaranteed.

[0042] Processing circuit unit 2 includes front-end electronics module 11, digital processing circuit module 9, and power board module 10.

[0043] Digital processing circuit module 9 includes signal processing unit 12 and processor circuit unit 13; power board module 10 includes secondary power supply unit 14 and high voltage power supply unit 15.

[0044] The front-end electronics module 11 amplifies and converts the detector output signal into digital data before it enters the signal processing unit 12. The signal processing unit 12 implements X-ray single-photon signal processing based on FPGA. The processor circuit unit 13 collects the detector's operating status and temperature, collects the signal processing unit 12's operating status and observed energy spectrum data, controls the power supply and power-on sequence of the signal processing unit 12, and realizes communication with the satellite platform.

[0045] The secondary power supply unit 14 provides power to the detector, and the high voltage power supply unit 15 provides the high voltage required for the detector to operate.

[0046] The low-energy detection module of the wide-spectrum, high dynamic range solar X-ray flare monitor employs a dual-channel design with two silicon drift (SDD) X-ray detectors and an effective detector area of ​​0.25 cm². 2 The observation window 7-1 uses a beryllium (Be) filter with a thickness of 200 μm, an observation energy range of 1-20 keV, an energy resolution better than 160 eV@5.9 keV, and a detection efficiency greater than 90%@5.9 keV. The dual-channel observation field of view is identical, designed to be ±2°. A movable baffle 6-1 is designed at the front end of the dual-channel detector. The baffle is made of a two-layer structure of copper (Cu) and aluminum (Al), with the copper material being 300 μm thick and the aluminum material 1 mm thick. The baffle has a central opening with a diameter of 0.8 mm. The baffle is driven by a motor 6-3 and can be positioned at the front end of the dual-channel detector. In normal observation mode, the movable baffle is positioned at either detector front end, resulting in two different effective observation areas for the dual-channel detector, one large and one small, each 0.25 cm². 2 and 0.005cm2 This design expands the dynamic observation range for solar eruptive activities such as flares of different magnitudes. When either detector fails, a baffle blocks the failed detector during periods of solar calm, allowing observations to be conducted using the normal detector. During solar flares, the baffle blocks the normal detector, limiting its effective observation area. This ensures high dynamic range observations of solar eruptive activities such as flares of different magnitudes even if either detector in the dual channels fails. The dual channels act as backups for each other, enhancing the instrument's reliability.

[0047] The high-energy detection module adopts a dual-channel design with two cadmium zinc telluride (CZT) detectors and an effective detector area of ​​4 cm². 2 The observation window 7-2 uses an aluminum (Al) filter with a thickness of 1 mm, covering an energy range of 20-700 keV. Its energy resolution is better than 8%@59.5 keV and 3%@662 keV, and its detection efficiency is greater than 90%@59.5 keV. Both channels have the same field of view, designed to be ±2°, and the same effective observation area of ​​4 cm². 2 Total 8cm 2 The dual-channel detector features a movable baffle 6-2 at its front end. The baffle is constructed of a two-layer structure of copper (Cu) and aluminum (Al), with the copper layer being 100 μm thick and the aluminum layer 1 mm thick. The baffle 6-3 is driven by a motor and can be positioned at the front end of the dual-channel detector. In normal observation mode, the movable baffle is positioned at either detector's front end, resulting in different detection efficiencies for the two channels. This expands the dynamic observation range for solar eruptions of varying magnitudes, such as flares, while simultaneously increasing the effective observation area and improving the sensitivity for observing high-energy X-rays from the sun. If either detector fails, the baffle blocks the failed detector during periods of solar calm, allowing observation using the normal detector. During solar flares, the baffle blocks the normal detector, limiting its detection efficiency. This ensures a high dynamic range for observing solar eruptions of varying magnitudes, even if either detector fails. The dual channels act as backups for each other, enhancing the instrument's reliability.

[0048] The functions of the solar X-ray flare monitor include:

[0049] (1) X-ray detection function: It has the functions of detecting solar X-ray energy spectrum and measuring time;

[0050] (2) Scientific data format arrangement function: The instrument receives the system time and satellite position information broadcast by the whole satellite, and arranges and frames the detected solar X-ray photon energy spectrum, instrument temperature and system time, satellite position and other information.

[0051] (3) Telemetry and remote control function: Under the scheduling of the satellite system, it has the function of telemetry data acquisition and sends telemetry parameters to the ground through the satellite computer, and receives remote control commands from the ground.

[0052] The solar X-ray flare monitor has the following operating modes:

[0053] Table 1 Operating Modes of the Solar X-ray Monitor

[0054]

[0055] Example

[0056] This invention relates to a low-energy detection module for a wide-spectrum, high dynamic range solar X-ray flare monitor, featuring a dual-channel X-ray silicon drift (SDD) detector with an effective area of ​​0.25 cm². 2 The observation window uses a 200 μm thick beryllium (Be) filter, covering an energy range of 1-20 keV with an energy resolution better than 160 eV at 5.9 keV and a detection efficiency greater than 90% at 5.9 keV. The dual-channel observation field of view is designed to be ±2°. The movable baffle at the front end of the dual-channel detector is a two-layer structure of copper (Cu) and aluminum (Al), with the copper material being 300 μm thick and the aluminum material 1 mm thick. The baffle has a central opening diameter of 0.8 mm. The effective observation area of ​​the dual-channel detector is 0.25 cm². 2 and 0.005cm 2 .

[0057] High-energy detection module: 2-channel cadmium zinc telluride (CZT) detector with an effective area of ​​4 cm². 2 The observation window uses a 1mm thick aluminum (Al) filter, covering an energy range of 20-700keV. The energy resolution is better than 8% at 59.5keV and 3% at 662keV, with a detection efficiency greater than 90% at 59.5keV. The dual-channel observation field of view is designed to be ±2°, with an effective observation area of ​​4cm². 2 Total 8cm 2 The movable baffle at the front end of the dual-channel detector is made of a two-layer structure of copper (Cu) and aluminum (Al), with the copper material having a thickness of 100μm and the aluminum material having a thickness of 1mm.

[0058] The solar X-ray flare monitor of this invention features an innovative modular design for its processing circuit unit. The multi-channel detectors, front-end electronics, and signal processing units are all designed as independent switches, so that a failure in any one channel will not affect the overall function of the instrument.

[0059] This invention relates to a solar X-ray flare monitor that receives system time and satellite position information broadcast by satellite. It then arranges and frames the detected solar X-ray photon energy spectrum, instrument temperature, system time, and satellite position information. The generated scientific observation data includes satellite position and ambient temperature information at the time of data acquisition, which is helpful for subsequent scientific data analysis.

[0060] Although the present invention has been disclosed above with reference to preferred embodiments, it is not intended to limit the present invention. Any person skilled in the art can make possible changes and modifications to the technical solutions of the present invention by utilizing the methods and techniques disclosed above without departing from the spirit and scope of the present invention. Therefore, any simple modifications, equivalent changes and alterations made to the above embodiments based on the technical essence of the present invention without departing from the content of the technical solutions of the present invention shall fall within the protection scope of the technical solutions of the present invention.

Claims

1. A wide-spectrum, high dynamic range solar X-ray flare monitor, characterized in that, It includes an X-ray probe unit (1) and a processing circuit unit (2). The X-ray probe unit (1) receives X-rays emitted by the sun, converts the light signal of the X-rays into an electrical signal, and sends the electrical signal to the processing circuit unit (2). The processing circuit unit (2) processes the received electrical signal and converts the electrical signal into X-ray information including energy and intensity, so as to realize the monitoring of solar X-ray flares with a wide energy spectrum and high dynamic range. The X-ray probe unit (1) includes a low-energy detection module and a high-energy detection module, both of which include an aperture (5), a movable baffle (6), an observation window (7) and a detector in sequence along the direction of sunlight; The low-energy detection module adopts a dual-channel design with two X-ray silicon drift detectors, and the observation window uses a beryllium filter. The observation fields of the two channels are the same. The high-energy detection module adopts a dual-channel design with two tellurium zinc cadmium detectors and aluminum filters in the observation window, with the two channels having the same field of view; In the normal observation mode of the low-energy detection module, the movable baffle is positioned at the front end of any X-ray silicon drift detector, so that the effective observation areas of the dual-channel detectors are large and small, in order to expand the dynamic observation range of solar eruption activities such as flares of different levels. When either detector fails, the active baffle blocks the failed detector when the sun is calm, and observations are conducted using the normal detector. When a solar flare occurs, the active baffle blocks the normal detector, limiting the effective observation area of ​​the normal detector. Thus, even if either detector in the dual channels fails, high dynamic range observations of solar flare activity of different levels can still be guaranteed. In the normal observation mode of the high-energy detection module, the movable baffle is positioned at the front end of either cadmium zinc telluride detector, so that the detection efficiency of the dual-channel detectors is different, thereby expanding the dynamic observation range of solar eruption activities for different levels of flares, while increasing the effective observation area and improving the observation sensitivity of solar high-energy X-rays. When either detector fails, the movable baffle blocks the failed detector when the sun is calm, allowing observations to be made using the normal detector; when a solar flare erupts, the movable baffle blocks the normal detector, limiting its detection efficiency. Thus, even if either detector in the dual channels fails, high dynamic range observations of solar eruption activity of different levels of flares can still be guaranteed.

2. The wide-spectrum, high dynamic range solar X-ray flare monitor according to claim 1, characterized in that, There are multiple apertures (5), each with a light-transmitting hole. The light-transmitting hole decreases in size along the direction of sunlight.

3. A wide-spectrum, high dynamic range solar X-ray flare monitor according to claim 2, characterized in that, The angle between the ray and the optical axis is 1°-30°.

4. A wide-spectrum, high dynamic range solar X-ray flare monitor according to claim 1, characterized in that, An active baffle (6) is set on the optical axis, and a filter is set in the observation window (7) to filter out light other than X-rays.

5. A wide-spectrum, high dynamic range solar X-ray flare monitor according to claim 1, characterized in that, The movable baffle is made of a two-layer structure of copper and aluminum. The movable baffle is driven by a motor and can be positioned at the front end of the dual-channel detector.

6. A wide-spectrum, high dynamic range solar X-ray flare monitor according to claim 1, characterized in that, The processing circuit unit (2) includes a front-end electronics module (11), a digital processing circuit module (9), and a power board module (10). The digital processing circuit module (9) includes a signal processing unit (12) and a processor circuit unit (13), and the power board module (10) includes a secondary power supply unit (14) and a high-voltage power supply unit (15). The front-end electronics module (11) amplifies and converts the detector output signal into digital and analog signals before it enters the signal processing unit (12). The signal processing unit (12) implements X-ray single-photon signal processing based on FPGA. The processor circuit unit (13) collects the detector's working status and temperature, collects the working status and observed energy spectrum data of the signal processing unit (12), controls the power supply and power-on sequence of the signal processing unit (12), and realizes communication with the satellite platform. The secondary power supply unit (14) provides power to the detector, and the high voltage power supply unit (15) provides the high voltage required for the detector to operate.

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