Moving Object Path Detection with Perpendicular Telescope Networks
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Solution Overview
Problem
Current methods for detecting and tracking space debris and other moving objects in space face challenges such as high costs, complexity, interference from external light sources, and difficulty in covering wide fields and accurately determining object paths, especially for objects in non-geostationary orbits and at low altitudes.
Innovation Solution
A system comprising multiple networks of telescopes with controlled orientations and fields of view, including networks in perpendicular planes and a conical segment, combined with image processing to estimate object paths, using Schmidt telescopes with large fields of view and photosensitive sensors.
Engineering Contradictions & Design Principles
Engineering Contradiction Analysis
1Area of stationary object
If a single telescope with wide field of view is used to cover large sky areas, then the detection coverage is improved, but the measurement precision of object path determination deteriorates
Solution Approach 1:
The detection system is segmented into multiple telescopes, each with a narrower field of view (1°-4°), arranged in networks covering different sky arcs. This segmentation allows each telescope to provide precise measurements while the collective network achieves wide coverage, resolving the contradiction between coverage area and measurement precision.
2Measurement precision
If multiple networks of telescopes are deployed to cover different sky arcs, then the object path determination precision is improved, but the device complexity increases
Solution Approach 1:
Multiple telescope networks observing different sky arcs are merged into a unified detection system with centralized coordination. The planes of different telescope networks are oriented perpendicular to each other, and their data are integrated to determine object paths, achieving high precision while managing complexity through systematic integration.
3Measurement precision
If telescopes with narrow field angles are used to achieve precise measurements, then the measurement precision is improved, but the detection coverage area deteriorates
Solution Approach 1:
The system transitions from a single-dimension approach (one telescope covering wide area) to a multi-dimensional approach (multiple telescopes in perpendicular planes covering different sky arcs). This dimensional expansion allows narrow-field telescopes to achieve precise measurements while the collective three-dimensional network provides comprehensive sky coverage.
Applied Scientific Principles
This section explains which scientific principles are used to turn an abstract innovation direction into a practical engineering solution.
Function Achieved in This Case
Enables efficient detection and path calculation of moving objects across various altitudes and orbits, reducing costs and complexity while minimizing interference from external light sources.
Implementation Method 1
Each of the telescopes being provided with a photosensitive sensor that periodically supplies an image I
Data Source
AI summary
A system for detecting the path of moving objects comprises: —A first network of N1 telescopes each having a field angle of M1 degrees and orientated to cover an arc of C° in a plane P1, M1 being between 1 and 4°, N1 being greater than C/M1, the observation angles ALPHAN1 of each of the telescopes being in a plane P1, —at least one second network of N2 telescopes each having a field angle of M2 degrees and orientated to cover an arc of C° in a plane P2, M2 being between 1 and 4°, N2 being greater than C/M1, the observation angles ALPHAN1 of each of the telescopes being in a plane P2 perpendicular to P1 comprising the observation axis of the stellar reference object, —the orientation of the telescopes being controlled to maintain the intersection between the planes P1 and P2 in the axis of a reference object, —at least a third network of N3 telescopes each having a field angle of at least M3 degrees and orientated to cover a conical segment of 360° with an elevation E3 between (180−C)/2°, M3 being between 1 and 4°, N3 being greater than 360/M3, —each of the telescopes being provided with a photosensitive sensor that periodically supplies an image I.