Golden star atmosphere microwave-submillimeter wave radiation transmission simulation method and system

Abstract

The invention provides a golden star atmosphere microwave-submillimeter wave radiation transmission simulation method and system, and the method comprises the steps: inputting golden star atmosphere profile data into an absorption coefficient calculation model, and obtaining the total absorption coefficient of each atmosphere layer of a golden star in combination with an observation frequency point and observation geometry of a golden star atmosphere microwave-submillimeter wave passive observation system; determining a radiation transmission path by using a ray tracing method in combination with the observation geometry of the aventurine atmosphere microwave-submillimeter wave passive observation system; obtaining the optical thickness of the atmosphere according to the absorption coefficient and the radiation transmission path; calculating the earth surface emissivity according to the Jinstar earth surface emissivity calculation model; the optical thickness and the surface emissivity of the atmosphere are utilized, radiation transfer integration is carried out based on a planet atmosphere generalized microwave radiation transfer theory, and brightness temperature simulation of the Jinxing atmosphere microwave-submillimeter wave passive observation system is carried out. The device and the method have the advantages that the 1-1000GHz microwave-submillimeter wave frequency band golden star atmosphere radiation transmission process can be accurately simulated.

Description

Technical Field

[0001] The present application belongs to the field of microwave remote sensing, and specifically relates to a method and system for simulating microwave-submillimeter wave radiation transmission in the atmosphere of Venus. Background Art

[0002] Unlike the Earth's atmosphere, the temperature and pressure of Venus' lower atmosphere are very high. The atmospheric pressure on the surface of Venus is about 93 standard atmospheres, and the surface temperature is about 470 degrees Celsius. This high temperature and high pressure environment will cause pressure-induced broadening of the spectral lines, and for non-nadir observations, the radiation transmission path needs to consider the effect of atmospheric refraction. Therefore, the existing radiation transmission model of the Earth's atmosphere is not applicable, and most of the existing radiation transmission models of the Venusian atmosphere are for the infrared-visible-ultraviolet frequency bands, and there are very few radiation transmission models for the microwave-submillimeter wave frequency bands, and these few models are only for the low-frequency microwave frequency band, or only for the submillimeter wave frequency band. Therefore, it is necessary to establish a radiation transmission model for the atmosphere of Venus. Summary of the invention

[0003] The purpose of this application is to overcome the defect of the lack of a calculation model for the radiation transmission of the Venus atmosphere in the microwave-submillimeter wave band.

[0004] In order to achieve the above objectives, the present application proposes a method for simulating microwave-submillimeter wave radiation transmission in the atmosphere of Venus, the method comprising:

[0005] Step S1) inputting the Venus atmospheric profile data into the absorption coefficient calculation model, combining the observation frequency and observation geometry of the Venus atmospheric microwave-submillimeter wave passive observation system, and calculating the total absorption coefficient of each atmospheric layer of Venus;

[0006] Step S2) using a ray tracing method in combination with the observation geometry of the Venus atmospheric microwave-submillimeter wave passive observation system to determine the radiation transmission path;

[0007] Step S3) calculating the optical thickness of the atmosphere according to the absorption coefficient and the radiation transmission path;

[0008] Step S4) calculating the surface emissivity according to the Venus surface emissivity calculation model and in combination with the radiation transmission path;

[0009] Step S5) Using the optical thickness of the atmosphere and the surface emissivity, radiation transfer integration is performed based on the generalized microwave radiation transfer theory of the planetary atmosphere to simulate the brightness temperature of the Venus atmospheric microwave-submillimeter wave passive observation system.

[0010] As an improvement of the above method, the Venus atmospheric profile data of step S1) includes: vertical distribution of temperature, pressure, sulfuric acid cloud density and gas concentration in the range of 0-130 km from the surface of Venus to the top of the atmosphere; the gases include: CO2, N2, SO2, CO, H2O, OCS, HDO, H2SO4, HCL, HF, NH3 and PH3.

[0011] As an improvement of the above method, the observation geometry of step S1) includes: satellite observation altitude and observation mode; the observation mode includes downward looking or limbus; if the observation mode is downward looking, the observation geometry also includes satellite zenith angle and azimuth angle; if the observation mode is limbus, the observation geometry also includes tangent altitude.

[0012] As an improvement of the above method, the calculation of step S1) to obtain the total absorption coefficient of each atmospheric layer of Venus includes:

[0013] Step S1-1), dividing the atmosphere of Venus within the altitude range of 0-130 km into 13-1300 layers;

[0014] Step S1-2), based on the atmospheric component spectral parameter information in the HITRAN spectral database, select appropriate line shape functions and spectral line broadening parameters, and calculate the total spectral line absorption coefficient of trace gases in each atmospheric layer by line-by-line integration method;

[0015] Step S1-3), based on the HITRAN absorption cross section database, calculate the continuous absorption coefficients of CO2 and N2 in each atmospheric layer;

[0016] Step S1-4), calculate the continuous absorption coefficient of water vapor in each atmospheric layer according to the following formula

[0017] Where, f represents frequency; T represents temperature; represents the partial pressure of carbon dioxide; represents the partial pressure of water vapor;

[0018] Step S1-5), calculate the absorption coefficient of sulfuric acid droplets in each atmospheric layer according to the following formula:

[0019]

[0020] Where M represents the cloud density, obtained from the atmospheric profile data of Venus; ρ represents the density of sulfuric acid liquid; ε' r and ε″ r Indicates intermediate parameters;

[0021] Step S1-6), the total spectral absorption coefficient of trace gases in each atmospheric layer, the continuous absorption coefficient of CO2, N2 and water vapor, and the absorption coefficient of sulfuric acid droplets are accumulated to obtain the total absorption coefficient of each atmospheric layer.

[0022] As an improvement of the above method, the number of layers of the Venus atmosphere, 13-1300 layers, and the layer heights are determined by the Venus atmospheric profile data, that is, if the Venus atmospheric profile data contains parameters of n atmospheric layers, the number of layers is n, and the layer height is the height difference between two adjacent atmospheric layers; or the atmosphere is evenly divided into n layers, each with the same layer height, and the temperature, pressure, sulfuric acid cloud density and gas concentration data of each atmospheric layer are obtained by interpolation of the Venus atmospheric profile data.

[0023] As an improvement of the above method, the selecting of a suitable linear function comprises:

[0024] For the atmosphere at 0-80km, select the Lorentz linear function; for the atmosphere at 80-110km, select the Voith linear function; for the atmosphere above 110km, select the Doppler linear function.

[0025] As an improvement of the above method, the selecting of appropriate line broadening parameters includes:

[0026] For SO2 and CO gases, if the simulated frequency band is 1-250 GHz, the CO2 broadening parameters measured in the laboratory under simulated Venusian atmospheric conditions are used; if the simulated frequency band is 250-1000 GHz, the CO2 broadening parameters of the HITRAN spectral database are used;

[0027] For H2O gas, the CO2 broadening parameters measured in the laboratory under simulated Venusian atmospheric conditions were used;

[0028] For H2SO4 gas, if the simulated frequency band is 1-250 GHz, the CO2 broadening parameters measured in the laboratory under simulated Venusian atmospheric conditions are used; if the simulated frequency band is 250-1000 GHz, the broadening parameters are set to 0;

[0029] For OCS, HCL, HF, and NH3 gases, the CO2 broadening parameters from the HITRAN spectral database were used;

[0030] For HDO gas, the air broadening parameter of the HITRAN spectral database is multiplied by 2.4 as its CO2 broadening parameter;

[0031] For PH3 gas, the CO2 broadening parameter uses 0.186 cm -1 atm -1 .

[0032] As an improvement of the above method, the calculation of the surface emissivity in step 4) includes:

[0033] Step S4-1), determining the longitude and latitude of the radiated Venus surface area according to the atmospheric radiation transmission path;

[0034] Step S4-2), according to the longitude and latitude of the Venus surface, using the global surface dielectric constant data of Venus obtained by the Magellan mission, the surface dielectric constant of the irradiated Venus surface area is obtained;

[0035] Step S4-3), calculate the surface emissivity ∈ according to the following formula:

[0036]

[0037] Among them, θ represents the angle of radiation incident on the ground, which is determined by the atmospheric radiation transmission path; ε represents the dielectric constant of the Venus surface; η represents the refractive index of the atmosphere immediately adjacent to the surface, which is obtained by the following formula:

[0038]

[0039] Among them, P1 represents the air pressure of the atmosphere close to the surface; T1 represents the temperature of the atmosphere close to the surface.

[0040] As an improvement of the above method, the step 5) comprises:

[0041] If the Venus atmospheric microwave-submillimeter wave passive observation system adopts downward-looking observation geometry, the observed brightness temperature T is calculated according to the following formula: B :

[0042]

[0043] Where f is the frequency; ∈ is the surface emissivity; T(z) is the vertical distribution of temperature with height z; T s Indicates the surface temperature; T c represents the cosmic background radiation; τ(x,y) represents the optical thickness of the atmosphere from point x to point y; κ a (f,z) represents the total atmospheric absorption coefficient of the atmosphere at an altitude of z when the frequency is f; θ represents the angle at which the radiation is incident on the ground, which is determined according to the atmospheric radiation transmission path;

[0044] If the Venus atmospheric microwave-submillimeter wave passive observation system adopts limb observation geometry, the observed brightness temperature T is calculated according to the following formula: B :

[0045]

[0046] The present application also provides a Venus atmosphere microwave-submillimeter wave radiation transmission simulation system, which is implemented based on the above method, and the system includes:

[0047] The absorption coefficient calculation module is used to input the Venus atmospheric profile data into the absorption coefficient calculation model, and calculate the total absorption coefficient of each atmospheric layer of Venus in combination with the observation frequency and observation geometry of the Venus atmospheric microwave-submillimeter wave passive observation system;

[0048] The radiation transmission path determination module is used to determine the radiation transmission path using the ray tracing method combined with the observation geometry of the Venus atmospheric microwave-submillimeter wave passive observation system;

[0049] The optical thickness calculation module is used to calculate the optical thickness of the atmosphere based on the absorption coefficient and the radiation transmission path;

[0050] The module for calculating the surface emissivity is used to calculate the surface emissivity based on the Venus surface emissivity calculation model and combined with the radiation transmission path;

[0051] The brightness temperature simulation module is used to simulate the brightness temperature of the Venus atmospheric microwave-submillimeter wave passive observation system by utilizing the optical thickness of the atmosphere and the surface emissivity and performing radiation transfer integration based on the generalized microwave radiation transfer theory of the planetary atmosphere.

[0052] Compared with the prior art, the advantages of this application are:

[0053] 1. The method of the present invention can accurately simulate the radiation transmission process of Venus atmosphere in the 1-1000GHz microwave-submillimeter wave frequency band

[0054] 2. The method of the present invention is not only applicable to the downward-looking Venusian atmospheric microwave-submillimeter wave passive observation system, but also to the limb observation system. In view of the difference in observation geometry between the downward-looking and limb observation systems, the present invention adopts different schemes to simulate the observed brightness temperature of the Venusian atmospheric microwave-submillimeter wave passive observation system. BRIEF DESCRIPTION OF THE DRAWINGS

[0055] Figure 1 Shown is a flow chart of the simulation method for microwave-submillimeter wave radiation transmission in the Venus atmosphere. DETAILED DESCRIPTION

[0056] The technical solution of the present application is described in detail below with reference to the accompanying drawings.

[0057] In response to the problem of the lack of a calculation model for the radiation transmission of the Venus atmosphere in the microwave-submillimeter wave frequency band, the present invention provides a method and system for simulating the microwave-submillimeter wave radiation transmission of the Venus atmosphere. The purpose is to achieve accurate simulation of the brightness temperature of the microwave-submillimeter wave passive observation system of the Venus atmosphere carried by the Venus orbiter. The method is not only applicable to downward-looking passive observation systems, but also to limb observation systems.

[0058] Example 1

[0059] like Figure 1 As shown, the present invention provides a method for simulating microwave-submillimeter wave radiation transmission in the atmosphere of Venus, comprising:

[0060] Step 1: Obtain the vertical distribution of temperature, pressure, sulfuric acid cloud density, and gas (including CO2, N2, SO2, CO, H2O, OCS, HDO, H2SO4, HCL, HF, NH3, and PH3) concentrations of each atmospheric layer in the range of 0-130 km from the surface of Venus to the top of the atmosphere.

[0061] Step 2: Obtain the observation frequency and observation geometry of the Venus atmospheric microwave-submillimeter wave passive observation system, where the observation geometry specifically includes the satellite observation altitude and observation mode (downward-looking or limb-looking). If it is a downward-looking observation, it also includes the satellite zenith angle and azimuth angle. If it is a limb-looking observation, it also includes the tangent altitude.

[0062] Step 3: Input the vertical distribution of temperature, pressure, and trace gas (including SO2, CO, H2O, OCS, HDO, H2SO4, HCL, HF, NH3, and PH3) concentration of each atmospheric layer in the range of 0-130 km from the surface of Venus to the top of the atmosphere into the spectral absorption coefficient calculation model, and calculate the total spectral absorption coefficient of each atmospheric trace gas at the observation frequency point.

[0063] The absorption coefficient calculation of the spectral line absorption coefficient calculation model in this step further includes the following processing method:

[0064] Step 3-1: Divide the atmosphere of Venus within the altitude range of 0-130km into i layers, where i ranges from 13 to 1300. The number of layers and layer heights of the atmospheric stratification can be determined by the atmospheric profile data of Venus, that is, if the atmospheric profile data of Venus contains the parameters of n atmospheric layers, the number of layers is n, and the layer height is the height difference between two adjacent atmospheric layers; the atmosphere can also be evenly divided into i layers, with the same layer height for each layer, and the temperature, pressure, sulfuric acid cloud density, and gas (including CO2, N2, SO2, CO, H2O, OCS, HDO, H2SO4, HCL, HF, NH3, and PH3) concentration data of each atmospheric layer can be obtained by interpolation from the atmospheric profile data of Venus.

[0065] Step 3-2: Select the appropriate line shape function. For the atmosphere of 0-80 km, use the Lorentz line shape; for the atmosphere of 80-110 km, use the Voith line shape; for the atmosphere above 110 km, use the Doppler line shape.

[0066] Step 3-3: Select appropriate line broadening parameters.

[0067] Step 3-3 includes the following processing methods:

[0068] Step 3-3-1: For SO2 and CO gases, if the simulated frequency band is 1-250 GHz, use the CO2 broadening parameters measured in the laboratory under simulated Venusian atmospheric conditions; if the simulated frequency band is 250-1000 GHz, use the CO2 broadening parameters of the HITRAN spectral database.

[0069] Step 3-3-2: For H2O gas, use the CO2 broadening parameters measured in the laboratory under simulated Venusian atmospheric conditions.

[0070] Step 3-3-3: For H2SO4 gas, if the simulated frequency band is 1-250 GHz, use the CO2 broadening parameters measured in the laboratory under simulated Venusian atmospheric conditions; if the simulated frequency band is 250-1000 GHz, set the broadening parameters to 0.

[0071] Step 3-3-4: For OCS, HCL, HF and NH3 gases, use the CO2 broadening parameters from the HITRAN spectral database.

[0072] Step 3-3-5: For HDO gas, multiply the air broadening parameter of the HITRAN spectral database by 2.4 as its CO2 broadening parameter.

[0073] Step 3-3-6: For PH3 gas, use 0.186cm for the CO2 broadening parameter -1 atm -1 .

[0074] Step 3-4: Based on the input atmospheric profile parameters and the spectral line center frequency, spectral line intensity, and transition low-state energy parameters of the HITRAN spectral database, combined with the linear function obtained in step 3-1 and the spectral line broadening parameters obtained in step 3-2, calculate the absorption coefficient of a single spectral line of a single gas in each atmospheric layer at the observed frequency point.

[0075] Step 3-5: Use the line-by-line integration method to calculate the absorption coefficient of all spectral lines of a single gas in each atmospheric layer at the observation frequency.

[0076] Step 3-6: Add up the absorption coefficients of all trace gases in the same atmospheric layer to obtain the total spectral line absorption coefficient of each atmospheric layer at the observation frequency.

[0077] Step 4: Input the vertical distribution of temperature, pressure, sulfuric acid cloud density, and gas (including CO2, N2, and water vapor) concentration of each atmospheric layer in the range of 0-130 km from the surface of Venus to the top of the atmosphere into the continuous absorption coefficient calculation model, and calculate the total continuous absorption coefficient of each atmospheric layer at the observation frequency.

[0078] The absorption coefficient calculation of the continuous absorption coefficient calculation model in this step includes the following processing methods:

[0079] Step 4-1: Based on the HITRAN absorption cross section database (CIA), calculate the continuous absorption coefficients of CO2 and N2 in each atmospheric layer.

[0080] Step 4-2: Calculate the continuous absorption coefficient of water vapor in each atmospheric layer according to the following formula;

[0081]

[0082] Where, f represents frequency, the unit is Hz; T represents temperature, the unit is K; Indicates the partial pressure of carbon dioxide in torr; Represents the partial pressure of water vapor in torr.

[0083] Step 4-3: Add the continuous absorption coefficients of CO2 and N2 and the continuous absorption coefficient of water vapor in the same atmospheric layer to obtain the total continuous absorption coefficient of each atmospheric layer at the observation frequency.

[0084] Step 5: Use the vertical distribution of temperature, pressure, and sulfuric acid cloud density of each atmospheric layer within the range of 0-130km from the surface of Venus to the top of the atmosphere to calculate the sulfuric acid droplet absorption coefficient of each atmospheric layer at the observation frequency according to the following formula

[0085]

[0086] Where f is the frequency in Hz; M is the cloud density in mg / m 3 ; ρ represents the density of sulfuric acid liquid, and its value is 1.84*10 9 ; ε' r and ε' r ' indicates an intermediate parameter.

[0087] Step 6: Add up the spectral line absorption coefficient, continuous absorption coefficient, and sulfuric acid droplet absorption coefficient of the same atmospheric layer calculated in steps 3-5 to obtain the total absorption coefficient of each atmospheric layer.

[0088] Step 7: According to Fresnel's refraction law, the refraction direction is determined by the following formula, and the radiation transmission path is determined by the ray tracing method;

[0089]

[0090] Among them, θ1 is the incident angle, the unit is rad; θ2 is the refraction angle, the unit is rad; ζ is the refractive index of the atmosphere where the refraction occurs, which is obtained by the following formula:

[0091]

[0092] Where P is the atmospheric pressure of the atmosphere where refraction occurs, in atm; T is the temperature of the atmosphere where refraction occurs, in K.

[0093] Step 8: Using the absorption coefficient and radiation transmission path calculated in steps 6 and 7, calculate the optical thickness τ of the atmosphere according to the following formula:

[0094]

[0095] Where τ(x,y) represents the atmospheric optical thickness from point x to point y; f represents the frequency; z represents the height; κ a (f,z) represents the total atmospheric absorption coefficient of the atmosphere at altitude z at frequency f.

[0096] Step 9: Calculate the surface emissivity based on the Venus surface emissivity calculation model and the atmospheric radiation transmission path determined in step 7;

[0097] This step further includes the following processing method:

[0098] Step 9-1: Based on the atmospheric radiation transmission path determined in step 7, determine the longitude and latitude of the radiated Venus surface area.

[0099] Step 9-2: Based on the longitude and latitude of the Venus surface, use the global surface dielectric constant data of Venus obtained by the Magellan mission to obtain the surface dielectric constant of the radiated Venus surface area.

[0100] Step 9-3: Calculate the surface emissivity ∈ according to the following formula:

[0101]

[0102] Among them, θ represents the radiation angle, which is determined according to the atmospheric radiation transmission path; ε represents the dielectric constant of the Venus surface; η is the refractive index of the atmosphere adjacent to the surface, which is obtained by the following formula:

[0103]

[0104] Where P1 is the air pressure of the atmosphere close to the surface, in atm; T1 is the temperature of the atmosphere close to the surface, in K.

[0105] Step 10: Using the atmospheric optical thickness and surface emissivity calculated in steps 8 and 9, perform radiation transfer integration based on the generalized microwave radiation transfer theory of planetary atmospheres and simulate the brightness temperature of the Venus atmospheric microwave-submillimeter wave passive observation system.

[0106] This step further includes the following processing method:

[0107] Step 10-1: If the Venus atmospheric microwave-submillimeter wave passive observation system adopts downward-looking observation geometry, the observed brightness temperature T is calculated according to the following formula: B :

[0108]

[0109] Where f represents frequency; ∈ represents the surface emissivity calculated in step 9; T(z) represents the vertical distribution of temperature with height z; T s Indicates the surface temperature; T c represents the cosmic background radiation, which is 2.7K; τ(x,y) represents the optical thickness of the atmosphere from point x to point y, which is calculated in step 8; κ a (f,z) represents the total atmospheric absorption coefficient of the atmosphere at altitude z at frequency f, calculated in step 6.

[0110] Step 10-2: If the Venus atmospheric microwave-submillimeter wave passive observation system adopts limb observation geometry, the observed brightness temperature T is calculated according to the following formula: B :

[0111]

[0112] Where f is the frequency; T(z) is the vertical distribution of temperature with height z; T s Indicates the surface temperature; T c represents the cosmic background radiation, which is 2.7K; τ(x,y) represents the optical thickness of the atmosphere from point x to point y, which is calculated in step 8; κ a (f,z) represents the total atmospheric absorption coefficient of the atmosphere at altitude z at frequency f, calculated in step 6.

[0113] In summary, the present embodiment provides a method for simulating microwave-submillimeter wave radiation transmission in the atmosphere of Venus, which is used to simulate the radiation transmission process in the atmosphere of Venus in the microwave-submillimeter wave frequency band of 1-1000 GHz, and to simulate the brightness temperature of a microwave-submillimeter wave passive observation system for downward or limb observation in the atmosphere of Venus.

[0114] Example 2

[0115] The present application also provides a Venus atmosphere microwave-submillimeter wave radiation transmission simulation system, which is implemented based on the above method, and the system includes:

[0116] The absorption coefficient calculation module is used to input the Venus atmospheric profile data into the absorption coefficient calculation model, and calculate the total absorption coefficient of each atmospheric layer of Venus in combination with the observation frequency and observation geometry of the Venus atmospheric microwave-submillimeter wave passive observation system;

[0117] The radiation transmission path determination module is used to determine the radiation transmission path using the ray tracing method combined with the observation geometry of the Venus atmospheric microwave-submillimeter wave passive observation system;

[0118] The optical thickness calculation module is used to calculate the optical thickness of the atmosphere based on the absorption coefficient and the radiation transmission path;

[0119] The module for calculating the surface emissivity is used to calculate the surface emissivity based on the Venus surface emissivity calculation model and combined with the radiation transmission path;

[0120] The brightness temperature simulation module is used to simulate the brightness temperature of the Venus atmospheric microwave-submillimeter wave passive observation system by utilizing the optical thickness of the atmosphere and the surface emissivity and performing radiation transfer integration based on the generalized microwave radiation transfer theory of the planetary atmosphere.

[0121] The present application may also provide a computer device, comprising: at least one processor, a memory, at least one network interface and a user interface. The various components in the device are coupled together through a bus system. It is understood that the bus system is used to achieve connection and communication between these components. In addition to the data bus, the bus system also includes a power bus, a control bus and a status signal bus.

[0122] The user interface may include a display, a keyboard or a pointing device, such as a mouse, a trackball, a touch pad or a touch screen.

[0123] It is understood that the memory in the embodiments disclosed in the present application may be a volatile memory or a non-volatile memory, or may include both volatile and non-volatile memories. Among them, the non-volatile memory may be a read-only memory (ROM), a programmable read-only memory (PROM), an erasable programmable read-only memory (EPROM), an electrically erasable programmable read-only memory (EEPROM), or a flash memory. The volatile memory may be a random access memory (RAM), which is used as an external cache. By way of example and not limitation, many forms of RAM are available, such as static random access memory (SRAM), dynamic random access memory (DRAM), synchronous dynamic random access memory (SDRAM), double data rate synchronous dynamic random access memory (DDRSDRAM), enhanced synchronous dynamic random access memory (ESDRAM), synchronous link dynamic random access memory (SLDRAM), and direct memory bus random access memory (DRRAM). The memories described herein are intended to include, but are not limited to, these and any other suitable types of memories.

[0124] In some embodiments, the memory stores the following elements, executable modules or data structures, or a subset thereof, or an extended set thereof: an operating system and applications.

[0125] The operating system includes various system programs, such as a framework layer, a core library layer, a driver layer, etc., which are used to implement various basic services and process hardware-based tasks. The application includes various application programs, such as a media player (Media Player), a browser (Browser), etc., which are used to implement various application services. The program for implementing the method of the embodiment of the present disclosure can be included in the application.

[0126] In the above embodiment, the processor may also call a program or instruction stored in the memory, specifically, a program or instruction stored in an application program, and is used to:

[0127] Execute the steps of the above method.

[0128] The above method can be applied to a processor or implemented by a processor. The processor may be an integrated circuit chip with signal processing capabilities. In the implementation process, each step of the above method can be completed by an integrated logic circuit of hardware in the processor or an instruction in the form of software. The above processor may be a general processor, a digital signal processor (Digital Signal Processor, DSP), an application specific integrated circuit (Application Specific Integrated Circuit, ASIC), a field programmable gate array (Field Programmable Gate Array, FPGA) or other programmable logic devices, discrete gates or transistor logic devices, discrete hardware components. The above-disclosed methods, steps and logic block diagrams can be implemented or executed. The general processor may be a microprocessor or the processor may also be any conventional processor, etc. The steps of the above-disclosed method can be directly embodied as a hardware decoding processor to execute, or the hardware and software modules in the decoding processor are combined to execute. The software module can be located in a mature storage medium in the field such as a random access memory, a flash memory, a read-only memory, a programmable read-only memory or an electrically erasable programmable memory, a register, etc. The storage medium is located in the memory, and the processor reads the information in the memory and completes the steps of the above method in combination with its hardware.

[0129] It is understood that the embodiments described in the present application can be implemented by hardware, software, firmware, middleware, microcode or a combination thereof. For hardware implementation, the processing unit can be implemented in one or more application specific integrated circuits (ASIC), digital signal processors (DSP), digital signal processing devices (DSPD), programmable logic devices (PLD), field programmable gate arrays (FPGA), general-purpose processors, controllers, microcontrollers, microprocessors, other electronic units for performing the functions described in the present application or a combination thereof.

[0130] For software implementation, the technology of the present application can be implemented by executing the functional modules (such as procedures, functions, etc.) of the present application. The software code can be stored in a memory and executed by a processor. The memory can be implemented in the processor or outside the processor.

[0131] The present application may also provide a non-volatile storage medium for storing a computer program. When the computer program is executed by a processor, each step in the above method embodiment can be implemented.

[0132] Finally, it should be noted that the above embodiments are only used to illustrate the technical solution of the present application and are not intended to limit it. Although the present application is described in detail with reference to the embodiments, a person skilled in the art should understand that any modification or equivalent replacement of the technical solution of the present application does not depart from the spirit and scope of the technical solution of the present application and should be included in the scope of the claims of the present application.

Claims

1. A method for simulating microwave-submillimeter wave radiation transmission in the atmosphere of Venus, comprising: Step S1) inputting the Venus atmospheric profile data into the absorption coefficient calculation model, combining the observation frequency and observation geometry of the Venus atmospheric microwave-submillimeter wave passive observation system, and calculating the total absorption coefficient of each atmospheric layer of Venus; Step S2) using a ray tracing method in combination with the observation geometry of the Venus atmospheric microwave-submillimeter wave passive observation system to determine the radiation transmission path; Step S3) calculating the optical thickness of the atmosphere according to the absorption coefficient and the radiation transmission path; Step S4) calculating the surface emissivity according to the Venus surface emissivity calculation model and in combination with the radiation transmission path; Step S5) Using the optical thickness of the atmosphere and the surface emissivity, radiation transfer integration is performed based on the generalized microwave radiation transfer theory of the planetary atmosphere to simulate the brightness temperature of the Venus atmospheric microwave-submillimeter wave passive observation system.

2. The method for simulating microwave-submillimeter wave radiation transmission in Venus atmosphere according to claim 1, characterized in that: The Venus atmospheric profile data of step S1) includes: vertical distribution of temperature, pressure, sulfuric acid cloud density and gas concentration in the range of 0-130 km from the surface of Venus to the top of the atmosphere; the gases include: CO2, N2, SO2, CO, H2O, OCS, HDO, H2SO4, HCL, HF, NH3 and PH3.

3. The method for simulating microwave-submillimeter wave radiation transmission in Venus atmosphere according to claim 1, characterized in that: The observation geometry of step S1) includes: satellite observation altitude and observation mode; the observation mode includes downward looking or limbal looking; if the observation mode is downward looking, the observation geometry also includes satellite zenith angle and azimuth angle; if the observation mode is limbal looking, the observation geometry also includes tangent altitude.

4. The method for simulating microwave-submillimeter wave radiation transmission in Venus atmosphere according to claim 1, characterized in that: The calculation of step S1) to obtain the total absorption coefficient of each atmospheric layer of Venus includes: Step S1-1), dividing the atmosphere of Venus within the altitude range of 0-130 km into 13-1300 layers; Step S1-2), based on the atmospheric component spectral parameter information in the HITRAN spectral database, select appropriate line shape functions and spectral line broadening parameters, and calculate the total spectral line absorption coefficient of trace gases in each atmospheric layer by line-by-line integration method; Step S1-3), based on the HITRAN absorption cross section database, calculate the continuous absorption coefficients of CO2 and N2 in each atmospheric layer; Step S1-4), calculate the continuous absorption coefficient of water vapor in each atmospheric layer according to the following formula Where, f represents frequency; T represents temperature; represents the partial pressure of carbon dioxide; represents the partial pressure of water vapor; Step S1-5), calculate the absorption coefficient of sulfuric acid droplets in each atmospheric layer according to the following formula: Where M represents the cloud density, obtained from the atmospheric profile data of Venus; ρ represents the density of sulfuric acid liquid; ε' r and ε″ r Indicates intermediate parameters; Step S1-6), the total spectral absorption coefficient of trace gases in each atmospheric layer, the continuous absorption coefficient of CO2, N2 and water vapor, and the absorption coefficient of sulfuric acid droplets are accumulated to obtain the total absorption coefficient of each atmospheric layer.

5. The method for simulating microwave-submillimeter wave radiation transmission in Venus atmosphere according to claim 4, characterized in that: The number of layers of the Venusian atmosphere, 13-1300 layers, and the layer heights are determined by the Venusian atmospheric profile data, that is, if the Venusian atmospheric profile data contains parameters of n atmospheric layers, the number of layers is n, and the layer height is the height difference between two adjacent atmospheric layers; or the atmosphere is evenly divided into n layers, each with the same layer height, and the temperature, pressure, sulfuric acid cloud density and gas concentration data of each atmospheric layer are obtained by interpolation of the Venusian atmospheric profile data.

6. The method for simulating microwave-submillimeter wave radiation transmission in Venus atmosphere according to claim 4, characterized in that: The selecting of suitable and linear functions comprises: For the atmosphere at 0-80km, select the Lorentz linear function; for the atmosphere at 80-110km, select the Voith linear function; for the atmosphere above 110km, select the Doppler linear function.

7. The method for simulating microwave-submillimeter wave radiation transmission in Venus atmosphere according to claim 4, characterized in that: The selecting of appropriate line broadening parameters comprises: For SO2 and CO gases, if the simulated frequency band is 1-250 GHz, the CO2 broadening parameters measured in the laboratory under simulated Venusian atmospheric conditions are used; if the simulated frequency band is 250-1000 GHz, the CO2 broadening parameters of the HITRAN spectral database are used; For H2O gas, the CO2 broadening parameters measured in the laboratory under simulated Venusian atmospheric conditions were used; For H2SO4 gas, if the simulated frequency band is 1-250 GHz, the CO2 broadening parameters measured in the laboratory under simulated Venusian atmospheric conditions are used; if the simulated frequency band is 250-1000 GHz, the broadening parameters are set to 0; For OCS, HCL, HF, and NH3 gases, the CO2 broadening parameters from the HITRAN spectral database were used; For HDO gas, the air broadening parameter of the HITRAN spectral database is multiplied by 2.4 as its CO2 broadening parameter; For PH3 gas, the CO2 broadening parameter uses 0.186 cm -1 atm -1 .

8. The method for simulating microwave-submillimeter wave radiation transmission in Venus atmosphere according to claim 1, characterized in that: The step 4) of calculating the surface emissivity comprises: Step S4-1), determining the longitude and latitude of the radiated Venus surface area according to the atmospheric radiation transmission path; Step S4-2), according to the longitude and latitude of the Venus surface, using the global surface dielectric constant data of Venus obtained by the Magellan mission, the surface dielectric constant of the irradiated Venus surface area is obtained; Step S4-3), calculate the surface emissivity ∈ according to the following formula: Among them, θ represents the angle of radiation incident on the ground, which is determined by the atmospheric radiation transmission path; ε represents the dielectric constant of the Venus surface; η represents the refractive index of the atmosphere immediately adjacent to the surface, which is obtained by the following formula: Among them, P1 represents the air pressure of the atmosphere close to the surface; T1 represents the temperature of the atmosphere close to the surface.

9. The method for simulating microwave-submillimeter wave radiation transmission in Venus atmosphere according to claim 1, characterized in that: The step 5) comprises: If the Venus atmospheric microwave-submillimeter wave passive observation system adopts downward-looking observation geometry, the observed brightness temperature T is calculated according to the following formula: B : T B (f)=e -τ(0,∞)secθ T s ∈+[1-∈]T c e -2τ(0,∞)secθ +secθ∫0 ∞ κ a (f,z)T(z)e -τ(z，∞)secθ dz+e -τ(0,∞)secθ [1-∈][∫0 ∞ secθκ a (f,z)T(z)e -τ(0,z)secθ dz] Where f is the frequency; ∈ is the surface emissivity; T(z) is the vertical distribution of temperature with height z; T s Indicates surface temperature; T c represents the cosmic background radiation; τ(x,y) represents the optical thickness of the atmosphere from point x to point y; κ a (f,z) represents the total atmospheric absorption coefficient of the atmosphere at an altitude of z when the frequency is f; θ represents the angle at which the radiation is incident on the ground, which is determined according to the atmospheric radiation transmission path; If the Venus atmospheric microwave-submillimeter wave passive observation system adopts limb observation geometry, the observed brightness temperature T is calculated according to the following formula: B : TB=T c θ -2τ(0,∞)secθ +secθ∫0 ∞ κ a (f,z)T(z)e -τ(z,∞)secθ d+e -τ(0,∞)secθ [∫0 ∞ secθκ a (f,z)T(z)e -τ(0,z)secθ d]。 10. A Venusian atmosphere microwave-submillimeter wave radiation transmission simulation system, implemented based on any of the methods described in claims 1-9, characterized in that: The system comprises: The absorption coefficient calculation module is used to input the Venus atmospheric profile data into the absorption coefficient calculation model, and calculate the total absorption coefficient of each atmospheric layer of Venus in combination with the observation frequency and observation geometry of the Venus atmospheric microwave-submillimeter wave passive observation system; The radiation transmission path determination module is used to determine the radiation transmission path using the ray tracing method combined with the observation geometry of the Venus atmospheric microwave-submillimeter wave passive observation system; The optical thickness calculation module is used to calculate the optical thickness of the atmosphere based on the absorption coefficient and the radiation transmission path; A module for calculating the surface emissivity, which is used to calculate the surface emissivity according to the Venus surface emissivity calculation model and combined with the radiation transmission path; and The brightness temperature simulation module is used to simulate the brightness temperature of the Venus atmospheric microwave-submillimeter wave passive observation system by utilizing the optical thickness of the atmosphere and the surface emissivity and performing radiation transfer integration based on the generalized microwave radiation transfer theory of the planetary atmosphere.

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