Rotational Collimating Assembly for Cassegrain Telescopes
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Solution Overview
Problem
Current methods for collimating Cassegrain telescopes, such as the star test and multi-beam laser alignment, are cumbersome and often require expensive equipment, making it difficult for amateur astronomers to achieve precise alignment, especially outdoors or in poor atmospheric conditions.
Innovation Solution
A rotational collimating assembly that allows the secondary mirror to be precisely rotated and adjusted about the optical axis, using radial markings and a reticle design in the eyepiece to measure misalignment in arc minutes, enabling precise collimation without external devices or stars.
Engineering Contradictions & Design Principles
Engineering Contradiction Analysis
1Ease of manufacture
If the star test method is used to collimate the telescope, then collimation can be performed with simple equipment, but the process becomes cumbersome and inaccurate due to the need to keep the star centered while simultaneously adjusting collimating screws
Solution Approach 1:
The patent introduces an artificial star as an intermediary object that can be positioned at the focal point and remains stationary during collimation. This intermediary eliminates the need to track and recenter a moving celestial star while adjusting collimating screws, thereby simplifying the operation without requiring complex computerized mounting systems.
Solution Approach 2:
The patent employs preliminary action by pre-positioning the artificial star at the focal point before collimation begins. This allows the collimation process to proceed without interruption, as the reference point remains fixed and eliminates the need for continuous recentering during screw adjustments.
2Measurement precision
If computer guided mounting is used to keep the star centered during collimation, then collimation accuracy improves, but the equipment cost increases significantly
Solution Approach 1:
The patent creates a simplified copy of a star using an artificial light source positioned at the focal point. This artificial copy provides all the necessary collimation reference functions without requiring expensive computerized tracking equipment, thereby achieving accurate collimation with simple, inexpensive tools.
Solution Approach 2:
The patent uses a simple, inexpensive artificial star that can be easily manufactured and positioned. This disposable or temporary reference object eliminates the need for expensive, complex computerized mounting systems while providing sufficient accuracy for collimation purposes.
3Adaptability or versatility
If atmospheric conditions are poor during star test collimation, then outdoor collimation becomes difficult, but indoor collimation with artificial star provides consistent results regardless of atmospheric conditions
Solution Approach 1:
The artificial star system is self-contained and does not depend on external atmospheric conditions. It provides its own light source and reference point, making the collimation process independent of weather, humidity, or air turbulence that would otherwise degrade the visibility of the Airy disk when using real stars.
Data Source
AI summary
Disclosed is a novel assembly and method that enables a user to collimate a focused Cassegrain telescope. The assembly, having a secondary mirror and support baffle, comprising an axle, a bearing, and hub, enables a user to precisely rotate or freely spin a Cassegrain telescope's secondary mirror about its optical axis. Incident to freely spinning the telescope's secondary mirror, the user may peer into the telescope's eyepiece and observe a focused image that may wobble, or remain stable, dependent upon how well the telescope's mirrors are aligned. Further, the assembly's eyepiece, comprising a reticle design, enables the observer to measure the magnitude and direction of image shift incident to the secondary mirror spinning. Lastly, the assembly, comprising a radially marked collimating faceplate, and radially marked collimating knob screws, enables a user to make specific adjustments to the telescope's secondary mirror, compensating for the observed image shift, precisely collimating the telescope.