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

More documents

Recommendations

Info

all of the checkpoints to be deemed that it makes it to the eyepiece. A diagram ofthese scenarios can be found in figure 4.5Figure 4.5: Scenarios of Rays Blocked by BafflesCase #1 is if the ray hits the back of the secondary mirror. If the secondary mirroris too large it will prevent the rays from hitting the primary mirror and entering theeyepiece. To calculate this, we determined the y-position of the ray at z=Z mirrors . Ifthe position was less than half the diameter of the secondary mirror then then theray is eliminated. In conclusion if equation 4.19 is true, then the ray is eliminated.b − tan α ≤ D 3(4.19)2Case #2 is that the ray hits the baffle attached to the secondary mirror be<strong>for</strong>ehitting the primary mirror. A line can be drawn from the secondary baffle corner tothe secondary mirror with the slope of m 1 and y-intercept of b 1 . It is assumed thecurvature in the secondary mirror in the z-direction is negligible. Thus, the algorithmdetermines when the line of the ray will intersect with the line of the secondary baffleat pos 2 . Then, if the position is in-between the start or end-position of the baffle thenthe intersection is real and the ray will be eliminated, if it is not in-between thenthe intersection will not occur. In conclusion, if equation 4.21 is true, then the ray iseliminated.m 1 = (Y 3 − D 32)(Z 3 − Z sch )(4.20)b 1 = Z 3 − m 1 Y 3 (4.21)17
pos 2 = (b − b 1)(m 1 − µ)(4.22)Z 3 ≥ pos 2 ≥ Z mirrors (4.23)Case #3 is that the ray hits the primary mirror, then hits the baffle attached tothe secondary mirror be<strong>for</strong>e hitting the secondary mirror. Similar to the past twoexamples, a line is drawn from the secondary baffle corner to the secondary mirrorwith m 1 and b 1 . The equation of the line coming off the primary mirror is known. Thealgorithm determines when the line of the ray will intersect the line of the secondarymirror. If the intersection occurs within the coordinates of the baffle then the raywill be eliminated. Thus, if equation 4.25 is true, then the ray will be eliminated.pos 3 = (a − b 1)(m 1 + k)(4.24)Z 3 ≥ pos 3 ≥ Z mirrors (4.25)Case #4 is that the ray hits the primary mirror, then hits the baffle attached tothe primary mirror. This was calculated similarly to the past examples. However,now the ray must hit the primary baffle instead of the secondary baffle. The baffleattached to the primary mirror is described with a slope of m 2 and y-intercept of b 2 .Finally, if equation 4.29 is true, then the ray will be eliminated.m 2 = (Y 1 − Deye2 )Z 1(4.26)b 2 = D eye2pos 4 = (a − b 2)(m 2 + k)(4.27)(4.28)Z 1 ≥ pos 4 ≥ 0 (4.29)Case #5 is that the ray hits the primary mirror and secondary mirror, then hits thebaffle on the primary mirror. If equation 4.33 is true, then the ray will be eliminated.m 3 = (Y 2 − l 2 )(s 2 − v)(4.30)b 3 = y 2 − m 3 s 2 (4.31)pos 4 = (b 2 − b 3 )(m 3 − m 2 )(4.32)18
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 and 10: Figure 3.2: Optical Layout of Newto
Page 11 and 12: Chapter 4Schmidt-Cassegrain Telesco
Page 13 and 14: Thus, the Airy Disk will include th
Page 15 and 16: Figure 4.3: Concentric Initial Ray-
Page 17: Table 4.1: Color, Wavelengths, and
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

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

Create successful ePaper yourself

Delete template?

Save as template?