Automatic Optimal Design Method for Axial and Side Supports of Primary Mirror of Large Field Astronomical Telescope
An automatic optimization technology for astronomical telescopes, applied in computing, special data processing applications, instruments, etc., can solve the problems of poor operability at the position of the support point, failure to extract the reflection surface of the main mirror, and poor operability, etc., to achieve Feasible and simple optimization design technology, shorten the design analysis cycle, and reduce the effect of analysis cost
Active Publication Date: 2016-08-31
ZIJINSHAN ASTRONOMICAL OBSERVATORY CHINESE ACAD OF SCI
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Problems solved by technology
[0003] At present, researchers have the following problems in the numerical calculation of the telescope's primary mirror: 1) The use of hyperstatically indeterminate supports forms an over-constrained
2) The position of the optimized support point is not practically operable, and there is no regularity and regularity
Since the grid is mostly divided freely, the position of the nodes is irregular, and the position of the optimized support point (must fall on the node) is also irregular, and the operability is not strong in the process of physical support.
3) The node information of the reflective surface of the primary mirror is not extracted for secondary development, and the root mean square error displayed is relative to the root mean square error of the mirror surface deformation in the original coordinate system
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Embodiment 1
[0057] Embodiment 1, the automatic optimal design method for the axial and side support of the primary mirror of a large-field astronomical telescope.
[0058] The finite element software chooses ANSYS, and the computer language is replaced by MATLAB. The specific implementation process is illustrated by taking the optimization process of the 2.5m astronomical telescope support as an example. Such as figure 1 Shown, select φ 1 =1000mm,φ 2 =2500mm, h=120mm, f=2.1316, D=φ 2 , connect the endpoints of the two parabolas to form a quadrilateral. The quadrilateral rotates 360 degrees around the y-axis to form a three-dimensional image of the main mirror of the 2.5m astronomical telescope.
[0059] The axial support adopts 54 points of three rings (inner ring regular dodecagonal vertices + middle ring regular octagonal vertices + outer ring regular twenty-four quadrangular vertices) statically determinate support, such as Figure 5 As shown, that is, the equal axial force is ap...
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The automatic optimization design method for the axial and side support of the main mirror of the large field of view astronomical telescope: based on a large-scale limited software platform: ⑴. Parametric modeling; ⑵. Parametric meshing; ⑶. Initial solution; ⑸. Set up an optimized solution target; ⑹. Automatically perform multiple cycles of steps ⑴-⑷; ⑺. Extract calculations for each cycle; Then proceed to step ⑼ and step ⑽ respectively: ⑼. Give the root mean square error; ⑽. Give the cloud map of the mirror deformation. The invention solves the design optimization problem of the support scheme of the main mirror of the large field of view telescope, and realizes that the primary mirror surface deformation RMS ERROR<10nm under the condition of axial support, and the main mirror surface deformation RMS ERROR<30nm under the condition that the side support zenith distance is 60 degrees. Provides a simple optimization design technology for the support of the primary mirror of the large-field astronomical telescope.
Description
technical field [0001] The invention relates to a method and technology for automatically optimizing the axial support and side support of the primary mirror of an astronomical telescope based on finite element software and computer language parameterized programming, belonging to the field of astronomical instrument research. Background technique [0002] Building a new generation of astronomical telescopes and improving the ability of large-scale sky surveys is one of the main trends in the development of ground optical equipment. Optical astronomical telescopes have high requirements on the reflective surface of the primary mirror. It has always been a cumbersome problem to optimize the root-mean-square error of the deformation of the primary mirror with axial support and side support under gravity to the order of nanometers. There are three ways to solve the support optimization problem of the main mirror of the astronomical telescope: one is the analytical method, that ...
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IPC IPC(8): G06F17/50
Inventor 杨戟王海仁程景全娄铮郑宪忠钱元
Owner ZIJINSHAN ASTRONOMICAL OBSERVATORY CHINESE ACAD OF SCI