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Instructions for an astronomy assignment where students use kepler's method to approximate mercury's orbit based on its maximum elongations. Students are required to draw tangent lines on a diagram of earth's orbit and then sketch in mercury's orbit, measuring its semi-major axis and eccentricity. A table of maximum elongations of mercury from 1967 to 1969.
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Astr 345 Assignment 4: Kepler’s method to find the orbit of Mercury
Due before midnight Fri, Sep 19, 2008 (full credit), before midnight Fri Sep 26, 2008 (half credit)
Introduction: Kepler’s method to find the orbit of Mercury uses the fact that we view Mercury’s orbit at a tangent when the planet is at its maximum elongation from the Sun. Given several maximum elongations, we can draw several tangent lines and therefore approximate the shape of the orbit. For this exercise, you will need a protractor and a good sharp pencil. Perform the exercise slowly and deliberately, and be as accurate as you can.
Set-up: Start by drawing a large circle, perhaps 5 cm in diameter. This circle represents the orbit of the Earth. Choose the center of the circle as being the location of the Sun (Earth’s orbital eccentricity is only 0.016, very close to circular). Draw a radius pointing horizontally to the right (i.e., towards “3 o’clock”). This line represents the direction of zero heliocentric longitude.
Draw tangent lines: Table 1 has 19 measurements of the maximum elongation of Mercury, every single occurrence in the years 1967-9. First, locate the Earth: choose a date, and move counterclockwise around the orbit by the number of degrees given. Place a dot to indicate the Earth’s location on that date.
Second, draw the tangent line. Draw a line away from Earth in a direction clockwise (west elongation) or counterclockwise (east elongation), by the number of degrees listed on Table 1. Be sure to use the Earth-Sun line as the zero for this angle.
The first date is done as an example in Figure 1.
Characterize the orbit: once you have drawn all 19 tangent lines, then sketch in Mercury’s orbit. Recall that the Sun is located at one focus. Draw in the major and minor axes. Measure the length of the semi-major axis, and scale this length to astronomical units (the Earth-Sun distance is 1 AU). Measure the eccentricity of the orbit. Compare your measured values with the accepted values for a and e (cite your source of information). Determine how close you are to the accepted values:
f ractional deviation =
measured − accepted accepted
Submit your diagram and complete calculations.
Grading:
Heliocentric Heliocentric Geocentric Date Longitude Elongation Date Longitude Elongation of Earth (deg) (deg) of Earth (deg) (deg) Feb 16, 1967 147 18 east Sep 20, 1968 357 26 east Mar 31, 1967 190 28 west Oct 31, 1968 037 18 west Jun 12, 1967 261 25 east Jan 13, 1969 113 18 east Jul 30, 1967 307 20 west Feb 23, 1969 154 26 west Oct 09, 1967 016 25 east May 06, 1969 225 21 east Nov 18, 1967 055 19 west Jun 23, 1969 271 23 west Jan 31, 1968 131 18 east Sep 03, 1969 340 27 east Mar 13, 1968 172 27 west Oct 15, 1969 021 18 west May 24, 1968 243 23 east Dec 28, 1969 096 19 east Jul 11, 1968 289 21 west
Table 1: Maximum elongations of Mercury 1967-
Figure 1: Top view of Earth’s orbit, drawing the line of sight to Mercury at its observed maximum elongation on Feb 16, 1967. The Earth’s longitude at the time was 147◦, and Mercury’s elongation was 18◦^ East. Eastwards is measured counterclockwise.