A method for predicting the spatial distribution of the top interface of the underground water-rich ice layer on Mars

Abstract

The present invention provides a method for predicting the spatial distribution of the top interface of the water-rich layer beneath Mars, relating to the field of planetary exploration. The method comprises: obtaining remote sensing images and elevation data of a study area, dividing the study area into several restricted areas, and calculating the apparent top interface position of the water-rich layer at the location of the rampart crater within each restricted area; extracting a central elevation profile of each restricted area, projecting the apparent top interface position of the water-rich layer at the location of the rampart crater onto the profile, and smoothly connecting relatively shallow projection points as the predicted top interface of the water-rich layer for each profile; and combining the predicted top interface of the water-rich layer from the extended area of ​​the study area and all elevation profiles to perform three-dimensional interpolation to obtain a predicted spatial distribution of the top interface of the water-rich layer within the study area. The present invention has the beneficial effect of accurately determining the spatial location and changing trend of the top interface of the water-rich layer beneath Mars, providing a scientific basis for better estimating the water ice reserves on Mars and rationally developing water ice resources.

Description

Technical Field

[0001] The present invention relates to the field of planetary exploration, and in particular to a method for predicting the spatial distribution of the top interface of a water-rich underground ice layer on Mars. Background Art

[0002] Research indicates that large quantities of water ice exist underground in the mid- and low-latitude regions of Mars (20°-50°). Studying the spatial distribution of groundwater ice in these regions not only helps us better understand ancient Martian climate change and trace the presence of life, but also provides a scientific basis for estimating Martian water ice reserves, thereby providing a crucial guarantee for securing water resources for future astronauts and colonists. While the European Space Agency's Mars Advanced Radar for Subsurface and Ionosphere Sounding (MARSIS) and the United States' Mars Orbiter Shallow Surface Radar (SHARAD) can detect the presence of groundwater ice on Mars, these radars can only predict the spatial distribution of groundwater ice layers with high water ice content (>60%) and have difficulty predicting the spatial distribution of groundwater-rich layers in areas with relatively low water ice content.

[0003] Rampart craters are a unique type of impact structure widely distributed on the Martian surface. They feature one or more layers of fluidized, continuous ejecta and are generally believed to be the product of the interaction between a subsurface water-ice-rich layer and a hypervelocity impactor. In other words, the impactor must have excavated water ice below the top of the subsurface water-ice-rich layer to form a rampart crater. Although the absolute age of rampart impacts at low latitudes on Mars spans a wide range (from 3.2 billion years ago to the present), most studies indicate that the top of the subsurface water-ice-rich layer has remained unchanged over this geological timeframe. Therefore, analyzing the distribution and excavation depth of rampart craters can provide key constraints on the spatial distribution of the top of the subsurface water-ice-rich layer on Mars. To predict the spatial distribution of the water-rich surface layer (BRI) in specific regions of Mars or globally by analyzing the distribution and excavation depth of rampart craters, previous methods primarily divide the study area into a series of grids (2°×2° or 5°×5°). The BRI craters with the smallest excavation depth are then selected from all the rampart craters within each grid. The excavation depth of each selected rampart crater represents the estimated depth of the BRI within that grid. However, this approach does not fully account for the spatial variation of the BRI within Mars. For example, some grids may lack rampart craters or have excavation depths significantly greater than those of surrounding craters. Consequently, it is impossible to ensure that the BRI estimates for each grid are consistent with the actual BRI. Furthermore, the BRI spatial distribution for the entire study area, obtained by combining the predicted BRI spatial distribution for all grids, is only a semi-quantitative estimate of the actual BRI spatial distribution and does not fully reflect the true spatial distribution of the BRI. Summary of the Invention

[0004] The present invention aims to address the problem that existing technologies have difficulty in reflecting the spatial location and changing trends of the top surface of the Martian underground water-ice layer. The present invention provides a method for predicting the spatial distribution of the top surface of the Martian underground water-ice layer. The method mainly includes the following steps:

[0005] S1. Obtain remote sensing images and elevation data of the study area, draw an elevation map of the area, and divide the study area into several restricted areas;

[0006] S2. Identify the barrier impact craters within each restricted area and calculate their distribution locations and diameters;

[0007] S3. Calculate the depth attribute of the Rampart crater and obtain the apparent top interface position of the underground water-ice-rich layer at the Rampart crater, specifically:

[0008] The depth attribute includes background elevation and excavation depth. The difference between the two is used as the apparent top interface of the underground water-rich ice layer at the location of the barrier crater.

[0009] S4. Extract the central elevation profile of each restricted area, project the barrier crater within the restricted area to the same elevation position of the central elevation profile according to the background elevation, and use the point below the projection point that is equal to the position of the apparent top interface of the underground water-rich ice layer at the location of the barrier crater as the projection point of the apparent top interface. Select the projection point of the underground water-rich ice top interface at the location of the shallowest barrier crater and connect them with a smooth line as the prediction result of the underground water-rich ice top interface of the central elevation profile of each restricted area;

[0010] S5. Obtain an extended area outside the study area, and process it using steps S2-S3 to obtain a prediction result of the apparent top interface of the underground water-ice-rich layer in the extended area;

[0011] S6. Perform three-dimensional interpolation on the predicted results of the apparent top interface of the underground water-rich ice layer in the combined expanded area and the predicted results of the top interface of the underground water-rich ice layer in the central elevation profile of each restricted area. Select the part covering the study area from the interpolation results to obtain the spatial distribution prediction results of the top interface of the underground water-rich ice layer in the study area.

[0012] Furthermore, the restricted area is divided by a series of curves in the regional elevation map that are approximately perpendicular to the elevation contour lines and are equally spaced.

[0013] Furthermore, barrier craters are identified based on the characteristics of fluid outflow, including three types: single-layer, double-layer, and multi-layer sputtering lace-type barrier craters.

[0014] Furthermore, the depth attributes of the rampart impact crater include background elevation and excavation depth;

[0015] The calculation steps of background elevation are as follows:

[0016] Draw a straight line in the east-west direction and a straight line in the north-south direction through the center of the Rampart crater. Extend the two curves to the outside of the outermost ejecta of the Rampart crater and stop. Extract the elevation data of the four stopping positions and take the average value as the background elevation of the Rampart crater.

[0017] The calculation formula for excavation depth is:

[0018]

[0019] in, Excavating the depth of Rampart Crater, represents the diameter of the Rampart crater, Indicates the conversion diameter of the impact crater. For the Martian rampart impact crater, The value is 6km.

[0020] Furthermore, the position of the apparent top interface of the underground water-ice-rich layer is calculated based on the depth properties of the barrier crater, specifically the difference between the background elevation and the excavation depth.

[0021] Furthermore, step S4 is specifically as follows:

[0022] S41, extracting the central elevation profile of each restricted area;

[0023] S42, projecting the barrier crater within the restricted area to a position at the same elevation as the central elevation profile according to the background elevation, and drawing a point below the projection point at the same elevation as the apparent top interface of the underground water-rich ice layer at the location of the barrier crater as the projection point of the top interface of the underground water-rich ice layer at that location;

[0024] S43. Along the central elevation profile, sequentially select the projection points of the top surface of the underground water-ice-rich layer at the location of the shallowest barrier crater, connect them smoothly, and use the resulting smooth curve as the prediction result of the top surface of the underground water-ice-rich layer at the central elevation profile of the restricted area;

[0025] S44. Repeat steps S42-S43 until the prediction result of the top interface of the underground water-rich ice layer of the central elevation profile in each restricted area is obtained.

[0026] Furthermore, the center elevation profile is specifically a profile that passes through the center of the restricted area and is parallel to the curve that divides the restricted area.

[0027] Furthermore, step S5 is specifically as follows:

[0028] S51. Expand the study area 100 km outward to form an additional area outside the edge as the expansion area, and extend the boundary lines of each restricted area and the expansion area to form several closed areas;

[0029] S52, for each closed area, processing is performed using steps S2-S3 until the apparent top interface position of the underground water-ice-rich layer at the location of the barrier crater in all closed areas is obtained;

[0030] S53. Select the minimum value from the positions of the apparent top interface of the underground water-rich ice layer at the location of the barrier impact crater in each closed area as the prediction result of the apparent top interface of the underground water-rich ice layer in the closed area, and use the obtained prediction results of the apparent top interface of the underground water-rich ice layer in all closed areas as the prediction results of the apparent top interface of the underground water-rich ice layer in the outward expansion restriction area.

[0031] Furthermore, step S6 is specifically as follows:

[0032] The prediction results of the apparent top interface of the underground water-rich ice layer in the expanded area and the prediction results of the top interface of the underground water-rich ice layer in the central elevation profile of each restricted area are combined for three-dimensional interpolation processing. The part covering the study area is selected from the interpolation results and the isobath map is drawn as the spatial distribution prediction result of the top interface of the underground water-rich ice layer in the study area.

[0033] A medium storing instructions and data for implementing a method for predicting the spatial distribution of the top interface of a water-rich underground ice layer on Mars.

[0034] A computer device comprises: a processor and the medium; the processor loads and executes instructions and data in the medium to implement a method for predicting the spatial distribution of the top interface of a water-rich underground ice layer on Mars.

[0035] The beneficial effects of the technical solution provided by the present invention are as follows: the present invention identifies all barrier craters in the study area based on the relationship between the barrier craters widely existing on the surface of Mars and the underground water-rich layer, and more accurately obtains the position of the apparent top interface of the underground water-rich layer where the barrier craters are located; extracts the central elevation profile in each restricted area, projects the position of the apparent top interface of the underground water-rich layer where the barrier craters are located onto the profile, and smoothly connects the relatively shallow projection points as the prediction result of the top interface of the underground water-rich layer on the profile, which truly and comprehensively reflects the spatial change trend of the top interface of the underground water-rich layer on Mars, and provides a scientific basis for better estimating the water ice reserves on Mars and rationally developing water ice resources. BRIEF DESCRIPTION OF THE DRAWINGS

[0036] The present invention will be further described below with reference to the accompanying drawings and embodiments, in which:

[0037] Figure 1 This is a flow chart of a method for predicting the spatial distribution of the top interface of a water-rich underground ice layer on Mars in an embodiment of the present invention;

[0038] Figure 2 is a schematic diagram of the research area in Chryse Planitia on Mars in an embodiment of the present invention;

[0039] Figure 3 is a spatial distribution diagram of the Chryse Planitia Rampart impact crater in an embodiment of the present invention;

[0040] Figure 4 is a schematic diagram of different types of barrier craters according to an embodiment of the present invention;

[0041] Figure 5 1 is a schematic diagram of a central elevation cross-sectional projection of a portion of a restricted area in an embodiment of the present invention;

[0042] Figure 6 : is a spatial distribution map of the elevation of the top surface of the underground water-ice-rich layer of Chryse Plain in an embodiment of the present invention;

[0043] Figure 7 This is a diagram verifying the depth of the top interface of the water-ice-rich layer underground in Chrysey Plain in an embodiment of the present invention;

[0044] Figure 8 It is a schematic diagram of the operation of the hardware device in the embodiment of the present invention. DETAILED DESCRIPTION

[0045] In order to have a clearer understanding of the technical features, purposes and effects of the present invention, specific embodiments of the present invention are now described in detail with reference to the accompanying drawings.

[0046] Embodiments of the present invention provide a method, device, and medium for predicting the spatial distribution of the top interface of a water-rich underground ice layer on Mars.

[0047] Please refer to Figure 1 , Figure 1 This is a flow chart of a method for predicting the spatial distribution of the top interface of a water-rich underground layer on Mars according to an embodiment of the present invention, which specifically includes the following steps:

[0048] The first step is to obtain remote sensing images and elevation data of the study area, draw a regional elevation map, and divide the study area into several restricted areas.

[0049] The research area selected in the embodiment of the present invention is located in Chryse Planitia on Mars, which is a circular plain close to the equator on the west side of the Tharsis Plateau. Figure 2 As shown, the center is located at 26.7°N, 320.0°E, with a diameter of approximately 1,800 kilometers and a depth of approximately 2.5 kilometers below the Martian geoid. Chryse Planitia exhibits surface features eroded by ancient Martian rivers: the Karsai Vallis flows from the Tharsis Plateau into Chryse Planitia, while the Ares Vallis and Tyr Vallis flow from the plateau east of Chryse Planitia into Chryse Planitia.

[0050] After determining the area of ​​Chryse Planitia on Mars, we obtained high-resolution CTX (Context Camera) mosaic images and MOLA (Mars Orbiter Laser Altimeter) elevation data covering the entire Chryse Planitia, and drew a geographic elevation map of the area. We then divided the study area into several smaller restricted areas using a series of curves that are approximately perpendicular to the elevation contour lines of the study area and are equally spaced (200 km apart), such as Figure 3 As shown, Figure 3This is a spatial distribution map of Chryse Planitia's rampart craters, based on an embodiment of the present invention. The base map is an elevation map based on MOLA data. In the figure, black, light, and dark dots represent single-layer, double-layer, and multi-layer sputtering lace-shaped rampart craters, respectively. Dark and light triangles represent rampart craters within and outside the margin of Chryse Planitia on Mars, respectively. The white dashed lines represent the boundaries dividing Chryse Planitia into different restricted areas, labeled P2, P4, P6, P8, P10, P12, P14, and P16, respectively.

[0051] In addition, the black solid line represents the central elevation profile of the restricted area to be extracted, which is marked as P1, P3, P5, P7, P9, P13, P15, and P17. The area within the dark circular dotted line is the study area, and the area enclosed by the outer light circular dotted line and the dark circular dotted line is the expansion area in the subsequent steps.

[0052] The second step is to identify the barrier craters within each restricted area and count their distribution locations and diameters.

[0053] The barrier craters are identified based on the characteristics of fluid outflow. All barrier craters within each restricted area are identified from high-resolution CTX (Context Camera) Mosaic images, such as Figure 4 As shown, the base image is a CTX (Context Camera) mosaic image with a resolution of 5 m / pixel. From left to right, they are single-layer, double-layer, and multi-layer sputtering barrier craters, which are used to identify all barrier craters within each restricted area in the figure.

[0054] The third step is to calculate the depth properties of the Rampart crater and obtain the position of the apparent top interface of the underground water-ice-rich layer where the Rampart crater is located.

[0055] The depth attributes for Rampart crater include background elevation and excavation depth:

[0056] The calculation steps of background elevation are as follows:

[0057] Draw a straight line in the east-west direction and a straight line in the north-south direction through the center of the Rampart crater. Extend the two curves to the outside of the outermost ejecta of the Rampart crater and stop. Extract the elevation data of the four stopping positions and take the average value as the background elevation of the Rampart crater.

[0058] The calculation formula for excavation depth is:

[0059]

[0060] in, Excavating the depth of Rampart Crater, represents the diameter of the Rampart crater, Indicates the conversion diameter of the impact crater. For the Martian rampart impact crater, The value is 6km.

[0061] The position of the apparent top interface of the underground water-rich ice layer is the predicted position of the top interface of the underground water-rich ice layer, which is calculated based on the depth properties of the barrier crater, specifically the difference between the background elevation and the excavation depth.

[0062] The fourth step is to extract the central elevation profile of each restricted area, project the barrier crater in the restricted area to the same elevation position of the central elevation profile according to the background elevation, and use the point below the projection point that is equal to the position of the apparent top interface of the underground water-rich layer at the location of the barrier crater as the projection point of the apparent top interface. The projection point of the underground water-rich layer at the location of the shallowest barrier crater is selected and smoothly connected as the prediction result of the underground water-rich layer top interface of the central elevation profile of each restricted area, specifically:

[0063] Step 1: Extract the center elevation profile of each restricted area. The center elevation profile is specifically: a profile that passes through the center of the restricted area and is parallel to the curve that divides the restricted area.

[0064] Step 2: Project the barrier crater in the restricted area to the same elevation position of the central elevation profile according to the background elevation, and draw a point below the projection point at the same elevation as the apparent top interface of the underground water-rich ice layer at the location of the barrier crater as the projection point of the top interface of the underground water-rich ice layer at that location.

[0065] like Figure 5 As shown, Figure 5 Schematic diagrams of projections of central elevation profiles of some restricted areas in an embodiment of the present invention, including (a) the P9 central elevation profile (corresponding to the restricted area defined by the P8 and P10 curves), (b) the P13 central elevation profile (corresponding to the restricted area defined by the P12 and P14 curves), and (c) the P5 central elevation profile (corresponding to the restricted area defined by the P4 and P6 curves).

[0066] Taking the P9 center elevation profile as an example, the black solid line is the depth contour of the apparent top interface of the underground water-rich ice layer along the center elevation profile. The indicated area is the center elevation profile. All the barrier craters in the restricted area are projected onto the P9 center elevation profile. When projecting, it is necessary to ensure that the projection point ( Figure 5The elevation of the point (the dot on the black solid line in a) is equal to the background elevation of the corresponding rampart crater, and the distance between the projection point and the corresponding rampart crater is less than 200 km. A point is drawn at a certain depth (equal to the excavation depth of the corresponding rampart crater) directly below each projection point to represent the position of the apparent top interface of the underground water ice-rich layer at that projection point. The blue, green, and red points correspond to different types of rampart craters, and the corresponding relationship is the same as Figure 3 consistent.

[0067] Step 3: along the central elevation profile, screen out the projection points of the underground water-rich top interface at the location of the shallowest barrier crater from the beginning to the end and connect them smoothly. The resulting smooth curve is used as the prediction result of the underground water-rich top interface of the central elevation profile of the restricted area ( Figure 5 dark curve in the .

[0068] Step 4: Repeat steps 2 to 3 to obtain Figure 3 The prediction results of the top interface of the underground water-rich layer at 8 central elevation profiles, including P1, P3, P5, P7, P11, P13, P15, and P17, indicated by the black solid lines.

[0069] The fifth step is to obtain the extended area of ​​the study area, and use the steps from the second to the third steps to process it to obtain the predicted results of the apparent top interface of the underground water ice-rich layer in the extended area.

[0070] In step 1, the study area was expanded 100 km outward to form an additional area outside the edge as the expansion area, and the boundary lines of each restricted area and the expansion area were extended to form several closed areas.

[0071] Step 2: For each closed area, process using steps S2-S3 until the apparent top interface position of the underground water-ice-rich layer at the location of the barrier crater in all closed areas is obtained.

[0072] Step three, select the minimum value from the positions of the apparent top interface of the underground water-rich ice layer at the location of the barrier crater in each closed area as the prediction result of the apparent top interface of the underground water-rich ice layer in the closed area, and use the obtained prediction results of the apparent top interface of the underground water-rich ice layer in all closed areas as the prediction results of the apparent top interface of the underground water-rich ice layer in the outward expansion restriction area.

[0073] The sixth step is to perform three-dimensional interpolation on the predicted results of the apparent top interface of the underground water-rich ice layer in the expanded area and the predicted results of the top interface of the underground water-rich ice layer in the central elevation profile of each restricted area. The part covering the study area is selected from the interpolation results to obtain the spatial distribution prediction results of the top interface of the underground water-rich ice layer in the study area.

[0074] The prediction results of the apparent top interface of the underground water-rich ice layer in the expanded area and the prediction results of the top interface of the underground water-rich ice layer in the central elevation profile of each restricted area are combined for three-dimensional interpolation processing. The part covering the study area is selected from the interpolation results and the isobath map is drawn as the spatial distribution prediction result of the top interface of the underground water-rich ice layer in the study area, such as Figure 6 As shown, Figure 6 1 is a spatial distribution map of the elevation of the top interface of the underground water-ice-rich layer of Chryse Plain in an embodiment of the present invention.

[0075] In order to verify the validity and accuracy of the spatial distribution prediction results of the top interface of the underground water-ice-rich layer in Chryse Planitia obtained by the present invention, the excavation depth of all rampart craters in Chryse Planitia can be used for verification. Since the elevation resolution of MOLA is 30 m, if the difference between the estimated depth of the top interface of the underground water-ice-rich layer at the location of the rampart crater and the excavation depth of the rampart crater is within the allowable error range (-30 m, this value is set according to the vertical resolution of MOLA of 30 m), it indicates that the estimated depth of the top interface is reasonable, otherwise, it indicates that the estimated depth is relatively unreasonable. If the estimated depth of the top interface of the underground water-ice-rich layer at the location of the rampart crater is unreasonable, add a white "×". Figure 7 As shown, the base map is an elevation map based on MOLA data. The dots correspond to different types of barrier craters, and the corresponding relationship is the same as Figure 3 Consistent. An “×” indicates that the error of the estimated depth of the top interface at that location is greater than the allowable error range, and no “×” indicates that the error of the estimated depth of the top interface at that location is within the allowable error range. The number of rampart craters whose elevation prediction results of the top interface of the underground water-rich ice layer in Chryse Planitia are within the allowable error range accounts for 90.1% of the total number of rampart craters, indicating that the method of the present invention has strong feasibility and robustness in predicting the spatial distribution of the top interface of the underground water-rich ice layer in Chryse Planitia. It should be noted that the prediction error of the top interface of the underground water-rich ice layer in some areas of Chryse Planitia is large and there are certain clustering characteristics, which may be due to the extremely uneven spatial distribution of the top interface of the underground water-rich ice layer. In general, the method of the present invention can accurately and finely predict the spatial distribution characteristics of the top interface of the underground water-rich ice layer in Chryse Planitia, and can be further applied to the prediction of the spatial distribution of the top interface of the underground water-rich ice layer in other areas of Mars in the future.

[0076] See Figure 8 , Figure 8 4 is a schematic diagram of the working of a hardware device according to an embodiment of the present invention. The hardware device specifically includes: a computer device 401, a processor 402 and a medium 403.

[0077] A computer device 401: The computer device 401 implements the method for predicting the spatial distribution of the top interface of the underground water-ice-rich layer on Mars.

[0078] Processor 402: The processor 402 loads and executes the instructions and data in the medium 403 to implement the method for predicting the spatial distribution of the top interface of the underground water-ice-rich layer on Mars.

[0079] Medium 403: The medium 403 stores instructions and data; the medium 403 is used to implement the method for predicting the spatial distribution of the top interface of the underground water-ice-rich layer on Mars.

[0080] The beneficial effects of the present invention are as follows: the present invention identifies all barrier craters in the study area based on the relationship between barrier craters widely existing on the surface of Mars and underground water-ice-rich layers, and more accurately obtains the position of the apparent top interface of the underground water-ice-rich layer where the barrier craters are located; extracts the central elevation profile in each restricted area, projects the position of the apparent top interface of the underground water-ice-rich layer where the barrier craters are located onto the profile, and smoothly connects the relatively shallow projection points as the prediction result of the top interface of the underground water-ice-rich layer on the profile, which truly and comprehensively reflects the spatial change trend of the top interface of the underground water-ice-rich layer on Mars, and provides a scientific basis for better estimating the water ice reserves on Mars and rationally developing water ice resources.

[0081] Finally, it should be noted that the above embodiments are only used to illustrate the technical solutions of the present invention, rather than to limit it. Although the present invention has been described in detail with reference to the aforementioned embodiments, those skilled in the art should understand that they can still modify the technical solutions described in the aforementioned embodiments, or make equivalent replacements for some of the technical features therein. However, these modifications or replacements do not deviate the essence of the corresponding technical solutions from the spirit and scope of the technical solutions of the various embodiments of the present invention.

Claims

1. A method for predicting the spatial distribution of the top interface of the underground water-rich ice layer on Mars, characterized in that: The specific steps include: S1. Obtain remote sensing images and elevation data of the study area, draw an elevation map of the area, and divide the study area into several restricted areas; S2. Identify the barrier impact craters within each restricted area and calculate their distribution locations and diameters; S3. Calculate the depth attribute of the Rampart crater and obtain the apparent top interface position of the underground water-ice-rich layer at the Rampart crater, specifically: The depth attribute includes background elevation and excavation depth, and the difference between the two is used as the apparent top interface position of the underground water-ice-rich layer at the location of the barrier crater; S4. Extract the central elevation profile of each restricted area, project the barrier crater within the restricted area to the same elevation position of the central elevation profile according to the background elevation, and use the point below the projection point that is equal to the position of the apparent top interface of the underground water-rich ice layer at the location of the barrier crater as the projection point of the apparent top interface. Select the projection point of the underground water-rich ice top interface at the location of the shallowest barrier crater and connect them with a smooth line as the prediction result of the underground water-rich ice top interface of the central elevation profile of each restricted area; S5. Obtain an extended area outside the study area, and process it using steps S2-S3 to obtain a prediction result of the apparent top interface of the underground water-ice-rich layer in the extended area; S6. Perform three-dimensional interpolation on the predicted results of the apparent top interface of the underground water-rich ice layer in the combined expanded area and the predicted results of the top interface of the underground water-rich ice layer in the central elevation profile of each restricted area. Select the part covering the study area from the interpolation results to obtain the spatial distribution prediction results of the top interface of the underground water-rich ice layer in the study area.

2. The method for predicting the spatial distribution of the top interface of the Martian underground water-ice-rich layer according to claim 1, characterized in that: The restricted area is divided by a series of curves in the regional elevation map that are approximately perpendicular to the elevation contour lines and are equally spaced.

3. The method for predicting the spatial distribution of the top interface of the Martian underground water-ice-rich layer according to claim 1, characterized in that: The barrier craters are identified based on the characteristics of fluid outflow, and include three types: single-layer, double-layer, and multi-layer sputtering lace-type barrier craters.

4. The method for predicting the spatial distribution of the top interface of the Martian underground water-ice-rich layer according to claim 1, wherein: The calculation steps of the background elevation are specifically as follows: Draw a straight line in the east-west and north-south directions through the center of the rampart crater, extend the two curves to the outside of the outermost ejecta of the rampart crater and stop, extract the elevation data of the four stopping positions, and take the average value as the background elevation of the rampart crater.

5. The method for predicting the spatial distribution of the top interface of the Martian underground water-ice-rich layer according to claim 1, wherein: The calculation formula of the excavation depth is specifically: in, Excavating the depth of Rampart Crater, represents the diameter of the Rampart crater, Indicates the conversion diameter of the impact crater. For the Martian rampart impact crater, The value is 6km.

6. The method for predicting the spatial distribution of the top interface of the Martian underground water-ice-rich layer according to claim 1, characterized in that: Step S4 is specifically as follows: S41, extracting the center elevation profile of each restricted area, specifically: a profile passing through the center of the restricted area and parallel to the curve dividing the restricted area; S42, projecting the barrier crater within the restricted area to a position at the same elevation as the central elevation profile according to the background elevation, and drawing a point below the projection point at the same elevation as the apparent top interface of the underground water-rich ice layer at the location of the barrier crater as the projection point of the top interface of the underground water-rich ice layer at that location; S43. Along the central elevation profile, sequentially select the projection points of the top surface of the underground water-ice-rich layer at the location of the shallowest barrier crater, connect them smoothly, and use the resulting smooth curve as the prediction result of the top surface of the underground water-ice-rich layer at the central elevation profile of the restricted area; S44. Repeat steps S42-S43 until the prediction result of the top interface of the underground water-rich ice layer of the central elevation profile in each restricted area is obtained.

7. The method for predicting the spatial distribution of the top interface of the Martian underground water-ice-rich layer according to claim 6, characterized in that: Step S5 is specifically as follows: S51. Expand the study area 100 km outward to form an additional area outside the edge as the expansion area, and extend the boundary lines of each restricted area and the expansion area to form several closed areas; S52, for each closed area, processing is performed using steps S2-S3 until the apparent top interface position of the underground water-ice-rich layer at the location of the barrier crater in all closed areas is obtained; S53. Select the minimum value from the positions of the apparent top interface of the underground water-rich ice layer at the location of the barrier impact crater in each closed area as the prediction result of the apparent top interface of the underground water-rich ice layer in the closed area, and use the obtained prediction results of the apparent top interface of the underground water-rich ice layer in all closed areas as the prediction results of the apparent top interface of the underground water-rich ice layer in the outward expansion restriction area.

8. The method for predicting the spatial distribution of the top interface of the Martian underground water-ice-rich layer according to claim 1, wherein: Step S6 is specifically as follows: The prediction results of the apparent top interface of the underground water-rich ice layer in the expanded area and the prediction results of the top interface of the underground water-rich ice layer in the central elevation profile of each restricted area are combined for three-dimensional interpolation processing. The part covering the study area is selected from the interpolation results and the isobath map is drawn as the spatial distribution prediction result of the top interface of the underground water-rich ice layer in the study area.

9. A medium, characterized in that: The medium storage instructions and data are used to implement a method for predicting the spatial distribution of the top interface of a water-rich underground ice layer on Mars as described in any one of claims 1 to 8.

10. A computer device, characterized in that: include: Processor and medium; the processor loads and executes instructions and data in the medium to implement a method for predicting the spatial distribution of the top interface of a water-rich underground ice layer on Mars as described in any one of claims 1 to 8.

Images