Design Optimization Model for a Schmidt-Cassegrain Telescope ME ...

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tical components as shown in figure 3.4. The location of these components are freewhich gives a large design space for the designer. The SCT system consists of twostrongly curved mirrors for our model. In addition, the Schmidt corrector helps reducethe about of loss light with respect to the traditional Cassegrain telescope. Thissystem will give us a very interesting optimization model as many different objectsand disciplines rely on the same design variables of the system.Figure 3.4: Optical Layout of Schmidt-Cassegrain Telescope without BafflesThe next chapter will explain the Schmidt-Cassegrain telescope model. It willgive an overview of the telescope and the model for each of the discipline subsystemscreated for this model.9
Chapter 4Schmidt-Cassegrain TelescopeThis chapter provides detail on the Schmidt-Cassegrain telescope algorithm and providesan overview of the analysis methods employed in this model.4.1 Schmidt-Cassegrain Telescope SystemThe Schmidt-Cassegrain Telescope(SCT) is a very popular telescope to amateur astronomers.It consists of two mirrors and a refractive medium, a Schmidt corrector.Due to the number of parts, the design space or configurations of the telescope canvary. This will give a more interesting design problem as there is a large amount ofspace to examine.Figure 4.1 is a picture of the Schmidt-Cassegrain telescope with our dimensioningof the design variables of the telescope. From this figure, all of the design variablesthat deal with the telescope and the baffle coordinates are shown in the z-y plane.It can be noted that zero of the z-axis begins at the location of the primary mirrorand the zero of the y-axis is at the center line and the x-plane goes into the paper.Also, the centerline shows that the system is symmetrical. The dimensioned tripodcan be found in figure 4.6. From the diagram, several geometric constraints can bedetermined. First, the length from the primary mirror to the Schmidt corrector mustbe greater than to the secondary mirror as shown in equation 4.1. Also, the innerdiameter of the tube is defined to be the diameter of the primary mirror. Thus, thediameter of the aperture stop and Schmidt corrector must be less than that or itwould be protruding through the tube as shown in equation 4.2.Z sch ≤ Z mirrors (4.1)D 1 ≥ D sch (4.2)The model comprises of several disciplines of the Cassegrain-Schmidt system.10
Page 1 and 2: Design Optimization Model for aSchm
Page 3 and 4: Chapter 2NomenclatureVariable Descr
Page 5 and 6: CRA slotCRB slotCRA stampCRB stampA
Page 7 and 8: in place. Next, telescopes include
Page 9: Figure 3.2: Optical Layout of Newto
Page 13 and 14: Thus, the Airy Disk will include th
Page 15 and 16: Figure 4.3: Concentric Initial Ray-
Page 17 and 18: Table 4.1: Color, Wavelengths, and
Page 19 and 20: pos 2 = (b − b 1)(m 1 − µ)(4.2
Page 21 and 22: ΣS I = ΣS II = ΣS III = 0 (4.35)
Page 23 and 24: (6) Location of the Schmidt correct
Page 25 and 26: The cost of manufacturing the eccen
Page 27 and 28: prices for spherical mirrors with v
Page 29 and 30: Figure 4.6: Schematic Drawing of Tr
Page 31 and 32: in equation 4.82. A parameter was a
Page 33 and 34: Table 5.1: Design Variables with Lo
Page 35: Bibliography[1] Ces selector versio

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