The assignment is attached in the following files. The data needed can be found in the second image labeled "data sheet".
jup_sm 1 The Revolution of the Moons of Jupiter Student Manual to Accompany the CLEA computer exercise Name_____________________ OFFICIAL USE ONLY 2 Historical Background We can deduce some properties of celestial bodies from their motions despite the fact that we cannot directly measure them. In 1543 Nicolaus Copernicus hypothesized that the planets revolve in circular orbits around the sun. Tycho Brahe (1546-1601) carefully observed the locations of the planets and 777 stars over a period of 20 years using a sextant and compass. These observations were used by Johannes Kepler, an assistant of Brahe’s, to deduce three empirical mathematical laws governing the orbit of one object around another. The addition of Isaac Newton’s law of gravity allows us to determine the mass of an object that is being orbited. Newton’s version of Kepler’s third law for a moon orbiting a much more massive parent body is: where M is the mass of the primary body, in units of the solar mass. d is the length of the semi-major axis of the elliptical orbit in units of the mean Earth-Sun distance, 1 A.U. (astronomical unit). If the orbit is circular (as will be assumed in this lab) the semi-major axis is the same as the radius of the orbit. p is the period of the orbit in Earth years. The period is the amount of time required for the moon to orbit the parent body once. In 1608 the telescope was invented, allowing the observation of objects not visible to the naked eye. Galileo used a telescope to discover that Jupiter had four moons orbiting it and made exhaustive studies of this system. The Jupiter system was especially important because it is a miniature version of the solar system which could be studied in order to understand the motions of the solar system. The Jupiter system provided clear evidence that Copernicus’ heliocentric model of the solar system was physically possible. Unfortunately for Galileo, the inquisition took issue with his findings; he was tried and forced to recant. 2 3 p dM = 3 Introduction We will observe the four moons of Jupiter that Galileo saw through his telescope. They are named Io (pronounced “eye-oh”), Europa, Ganymede and Callisto (in order of distance from Jupiter). The moons appear to be lined up because we are looking edge-on to the orbital plane of the moons of Jupiter (see Figure 1). As time goes by, the moons will move about Jupiter. Although the moons move in roughly circular orbits, you can only see the perpendicular distance of each moon to the line of sight between Jupiter and Earth. Therefore, the perpendicular distance of the moon should be a sinusoidal curve if you plot it versus time (see Figure 2). By taking enough measurements of the position of a moon, you can fit a sine curve to the data and determine the radius of the orbit (the amplitude of the sine curve) and the period of the orbit (the period of the sine curve). Once you know the radius and period of the orbit of that moon and convert them into appropriate units, you can determine the mass of Jupiter by using Kepler’s Third law. You will determine Jupiter’s mass for each of the four moons; there will be errors of measurement associated with each moon, therefore your Jupiter masses may not be exactly the same. The Jupiter program simulates the operation of an automatically controlled telescope with a charge-coupled device (CCD) camera that provides a video image to a computer screen. It is a sophisticated computer program that allows convenient measurements to be made at a computer console, as well as adjusting the telescope’s magnification. The computer simulation is realistic in all important ways, and using it will give you a good feel for how astronomers collect data and control their telescopes. Instead of using a telescope and actually observing the moons for many days, the computer simulation shows the moons to you as they would appear if you were to look through a telescope at the specified time. APPARENT POSITION OF A MOON The apparent position of a moon varies sinusoidally with the changing angle form the line of sight as it orbits Jupiter. Here the apparent position is measured in units of the radius of the moon’s orbit and the angle measured in degrees. Figure 1 4 Overall Strategy This is the overall plan of action for this laboratory exercise: • Use the CLEA Jupiter program to observe and measure the apparent positions of the moons of Jupiter. • Plot your observations for each moon on the appropriate graph paper supplied with this write- up. • Carefully sketch in the curve (sine curve) best representing the data on each graph. • Determine the period and semi-major axis for the orbit of each moon form its graph, then convert the values to years and AUs, respectively. • Calculate the mass of Jupiter from your observations of each moon, then determine the average value for Jupiter’s mass form your individual values. Installing and Running the CLEA Jupiter Software 1. Once you have downloaded the software package for the CLEA Jupiter program, it will appear as a file called “JupLab”. 2. Double click on this icon or file name and a self-extracting program will run. This program will install the software on your computer. Follow the instructions that are shown to you. 3. Once the program is finished installing, there will be an icon located on your desktop that looks like this: 4. Double click this icon. This should bring up a starting screen with a list of menu items across the top. Using the Jupiter Program 1. Open the Jupiter program by double-clicking on it with the mouse. The first screen should look like this: 5 You must first select “File” then “Log In” from the menu before taking data. A popup window will appear that looks like this: DO NOT ENTER ANYTHING IN THIS WINDOW! 2. Click “OK” to continue. The program will show you a warning box that looks like this: simply click “OK” and continue. 3. The next screen will look like this: 6 4. Select “File” then “Run”. The next dialog box to appear is Set Date/Time. There is nothing to change for this box. 5. Click “OK” to continue. 6. Select “File” then “Timing” to set up the time interval. The next dialog box to appear is Timing Intervals. The observational time interval will need to be changed to 12 hours. 7. Click “OK” to continue. 7 8. The next screen should look like this: 9. You can display the screen at four scales of magnification by clicking on the 100X, 200X, 300X and 400X buttons at the bottom of the screen. In order to improve the accuracy of your measurement of a moon, you should use the largest possible magnification that still leaves the moon on the screen. 10. In order to measure the perpendicular distance of each moon from Jupiter, move the pointer until the tip of the arrow is centered on each moon and click the mouse. Information about the moon will appear at the lower right corner of the screen. This includes the name of the selected moon, the x and y pixel location on the screen, and the perpendicular distance (in units of Jupiter’s diameter) from the Earth-Jupiter line of sight for the selected moon as well as an E or W to signify whether it is east or west of Jupiter. If the moon’s name does not appear, you did not center the arrow exactly on the moon; try again. Jupiter is in the center of the screen, while the small point-like moons are to either side. Sometimes a moon is behind Jupiter, so it cannot be seen. Even at high magnifications, they are very small compared to Jupiter. The current telescope magnification is displayed at the upper left hand corner of the screen. The date, UT (the time in Green- wich, England) and J.D. (Jupiter’s diameter in A.U.) are displayed at the lower left hand corner of the screen. 8 Click on each of the moons to find the number of J.D. (Jupiter diameters) the moon is away from the center of Jupiter. Notice the edge on Jupiter is 0.5 J.D. To measure each moon accurately, switch to the highest magnification setting that leaves that moon on the screen. If the moon is behind Jupiter, record the distance for that moon as zero. Below is an example of how to record your data: Example: (1) Date (2) Time (3) Day (4) Io (5) Europa (6) Ganymede (7) Calisto 7/24 0.0 1.0 +2.95 +2.75 -7.43 +13.15 7/24 12.0 1.5 -0.86 +4.7 -6.3 +13.15 Column 1: Local Date Column 2: Universal Time Column 3: Day - number of day (e.g. 1.0, 1.5, 2.0, ...) NOT counting cloudy days. Enter cloudy days in the space provided at the bottom of the data sheet. Columns 4-7: Record each moon’s position under the column for that moon. Use + for west and - for east. For example: If Europa were selected and had an X = 2.75W, you would enter that in column 5 as +2.75. 11. When you have recorded the Universal Time and the perpendicular distances for every moon, you may make the next set of observations by clicking on the Next button. 12. When a new screen appears, be sure to return to 100X zoom and repeat steps 9 – 11. 13. When you have finished taking all of the necessary readings, you may quit the program by selecting “Quit”. Cloudy Days In reality, astronomers often have to deal with