Telescope effect

ABS polymer exhibits a telescope effect at room temperature, but not at lower temperatures. 

The telescope effect is observed with practically all polymers, including X-ray amorphous polymers. One of the few exceptions is cellulose acetate. Necking can often be prevented by very slow stretching. The difference between the brittleness temperature and the experimental temperature is... 

Something else should be said about the impact of accommodation- When the (general) theory concerned is strongly supported independently of the fact at issue, the accommodation of some fact, even in this ad hoc way, may well still supply the best explanation that science can currently supply for that fact. So, for example, the best explanation in, say, 1700 for the observation of no stellar parallax was surely the Copemican one—that there must in fact be an apparent parallactic motion but that even the nearest stars are so far away as to make the effect too small to be detected by even the best available telescopes. (Here, as before with Ptolemy and with scientific creationism, we use the phenomenon—no observed parallax—to fix (in this case in a rather loose way) an otherwise free parameter in the theory (distance to the nearest star).)... 

In astronomy, we are interested in the optical effects of the turbulence. A wave with complex amplitude U(x) = exp[ irefractive index, resulting in a random phase structure by the time it reaches the telescope pupil. If the turbulence is weak enough, the effect of the aberrations can be approximated by summing their phase along a path (the weak phase screen approximation), then the covariance of the complex amplitude at the telescope can be shown to be... 

Evolution in telescope making since the Palomar has not been limited to the area of optical production. The alt-azimuthal mount has become the established solution since the Bolshoi 6 m telescope, for its superior mechanical performance and the compact, cost-efficient enclosure design it allows. Better understanding of the properties of atmospheric turbulence allowed a more accurate characterization of a telescope properties, a more balanced approach towards specifications and error budgeting and a better understanding of the utmost importance of site selection. Any ground-based telescope of appreciable size will be primarily limited by the effect of atmospheric turbulence, not to mention the proportion of photometric nights allowed by weather conditions. 

Edge effects must be considered carefully since there are so many interior edges with a segmented mirror telescope. Again several approaches have been considered. The approach used for the Keck segments was to pohsh the mir-... 

The very first question that comes to mind when dealing with giant telescopes is the cost-effective feasibility of its optics. Assuming classical materials for the segments blanks, however, there is no need for a very substantial increase in production capacity from existing suppliers provided that the segment size remains below 2-m. Moderately lightweight Silicon Carbide is also considered as a serious and potentially cost-effective candidate, for its superior thermal performance and specific stiffness. 

Abstract Detectors play a key role in an astronomical observatory. In astronomy, the role of the telescope and instrument is to bring light to a focus - in effect, the telescope-instrument act as spectacles . The detectors, meanwhile, have the critical role of sensing the light - the detectors are the eyes of an observatory. The performance of an astronomical observatory is directly dependent upon the performance of its detector systems. 

Stability. All spectrographs are subject to structural deformation due to thermal effects or, in the case of instmments mounted directly on the telescope, variation in the gravity vector. This can be divided into two parts. 

Spot size. The size of the LGS is a critical issue, since it dehnes the saturation effects of the laser and the power needed to reach a given system performance, and also the quality of the wavefront sensing. There is an optimum diameter of the projector, because, if the diameter is too small, the beam will be spread out by diffraction and if it is too large it will be distorted due to atmospheric turbulence. The optimum diameter is about 3ro, thus existing systems use projection telescopes with diameters in the range of 30-50 cm. 

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