Chapter 64Examination of ParallaxKepler can demonstrate the possible maximum parallax of Mars. He will reperform the calculations and comparisons of chapters 61 and 62 with parallax, and show that the results do not accord with reason.
Chapter 61 CalculationIn chapter 61, Kepler found the nodes to be exactly opposite each other in zodiacal position: 16° 46^{1}/_{3}′ Taurus and Scorpio. When he recalculates the location of the nodes, incorporating a slight parallax of 1′ to 2′ in his observations, he finds the nodes to be at 16¼° Taurus and 17¾° Scorpio. Thus, the use of a parallax correction causes the nodes not to be opposite each other, which is impossible of the plane of the Martian orbit intersects the body of the sun. Chapter 62 CalculationThis concerns calculating the theoretical latitude of Mars, and comparing it with the observations. Compare the calculated latitudes in chapter 62 with the observed latitudes from chapter 15. Choosing years for which parallax was taken into account in formulating the table of chapter 15, Kepler reconsiders the observations, without the parallax correction he had previously made. (This explains the two values for latitude from chapter 15 in the table in chapter 62.) It is consistently true that not making a correction for parallax gives values that better agree with his theory:
ConclusionThus, it is true that the parallax is very small, not to exceed 2 or 2½ minutes, which is within the limits of the Brahean observations. Using this parallax would require a change of half a minute to the inclination, making it 1°51′. Afterword:A rough calculation of the maximum parallax of Mars, using modern data for the ratio of the body of the earth to its orbit (unavailable to Kepler), gives a maximum possible parallax at opposition of around ½′. These are the numbers used:
The mean earthsun distance is 92,960,000 miles, which puts the sunearth distance as 92,960,000 / 3963 ~ 23,500 semidiameters of the earth. Compare this with Kepler’s estimate of 7002000 semidiameters in chapter 11. Interestingly, with better astronomical equipment and improved accuracy of observations, the more exact determination of parallax allowed the calculation of astronomical distances. Can you think of how this was done?
