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Jupiter Mass CESAR Science Case Jupiter Mass Calculating a planet’s mass from the motion of its moons Student’s Guide Mass of Jupiter 2 CESAR Science Case Table of Contents The Mass of Jupiter ........................................................................... ¡Error! Marcador no definido. Kepler’s Three Laws ...................................................................................................................................... 4 Activity 1: Properties of the Galilean Moons ................................................................................................. 6 Activity 2: Calculate the period of your favourite moon ................................................................................. 9 Activity 3: Calculate the orbital radius of your favourite moon .................................................................... 12 Activity 4: Calculate the Mass of Jupiter ..................................................................................................... 15 Additional Activity: Predict a Transit ............................................................................................................ 16 To know more… .......................................................................................................................... 19 Links ............................................................................................................................................ 19 Mass of Jupiter 3 CESAR Science Case Background Kepler’s Three Laws The three Kepler’s Laws, published between 1609 and 1619, meant a huge revolution in the 17th century. With them scientists were able to make very accurate predictions of the motion of the planets, changing drastically the geocentric model of Ptolomeo (who claimed that the Earth was the centre of the Universe) and the heliocentric model of Copernicus (where the Sun was the centre but the orbits were perfectly circular). These laws can be summarised as follows: 1. First Law: The orbit of every planet is an ellipse, with the Sun at one of the two foci. 2. Second Law: A line joining a planet and the Sun sweeps out equal areas during equal intervals of time. Figure 1: Second Law of Kepler (Credit: Wikipedia) 3. Third Law: The square of the orbital period of a planet is directly proportional to the cube of the semi-major axis of its orbit. Considering that the planet moves in a circular orbit with no friction, the gravitational force equalizes the centrifugal force. Therefore, the third Kepler’s law can be express as: 퐺푀푚 퐹 = 퐹 → = 푚 푎 퐺 퐶 푅2 푐 푣2 퐺푀푚 푣2 푎푛푑 푎푠 푎 = → = 푚 푐 푅 푅2 푅 2휋 푎푠 푣 = 휔 ∙ 푅 = 푅 푇 Note that 푀 is the mass of the main object and 푚 is the mass of the orbiting one, 푣 is the linear velocity of the moving body, 푅 is the radius of the orbit, 휔 is the angular velocity of it, 푇 is the period of the orbiting object (in seconds) and 퐺 is the gravitational constant, which value is 퐺 = 6.674 ∙ 10−11 푚3 푘푔−1 푠−2 Mass of Jupiter 4 CESAR Science Case Therefore, the quotation previously mentioned is achieved: 푇2 ∝ 푅3 퐺푀 푅3 = 4휋2 푇2 In this Science Case we are going to make use of two of the most practical astronomical tools: Cosmographia and Stellarium. By applying the third Law of Kepler we could calculate the mass of Jupiter. Please check CESAR Booklets (see links) to know how to install and configure these software packages. Did you know? Jupiter is the largest planet in the Solar System: more than 11 times bigger than the Earth and around of 320 times heavier than it. Jupiter is also the planet with more moons orbiting around it: 79 moons have been discovered up to 2018. However these moons are not equal in size. The biggest ones (Io, Europa, Ganymede and Callisto) were the first discovered by Galileo Galilei in 17th century. It was in Galileo’s honour why they are called the Galilean Moons. Figure 2: The Galilean moons (Credits:NASA) Mass of Jupiter 5 CESAR Science Case Activity 1: Properties of the Galilean Moons For this first activity Cosmographia will be used. 1. Double click on “Cosmographia.app” and it will pop up the application as Figure 3. Figure 3: Cosmographia starting view Note: The menu of Cosmographia is at the left part of the window. 2. Select the first option (the white circles). The image of the solar system bodies will be displayed. See Figure 4 Figure 4: Solar System bodies as seen in Cosmographia Mass of Jupiter 6 CESAR Science Case 3. Find out Jupiter and click on it. Cosmographia will drive you to Jupiter (Figure 5) Figure 5: Solar System bodies 4. Scroll out and turn the mouse until you find the Galilean moons (Io, Europa, Ganymede and Callisto), as in Figure 6 Figure 6: Solar System bodies as seen in Cosmographia Mass of Jupiter 7 CESAR Science Case 5. Display the trajectory for the four moons by doing right click on each one (see Figure 7) Figure 7: Trajectory toggle menu as seen in Cosmographia 6. Display the properties of Jupiter and every Galilean moons and will Table 1 Figure 8: Right click on Jupiter (left image); Jupiter properties (right image) as seen in Cosmographia Mass of Jupiter 8 CESAR Science Case Now is your turn to write down the most important properties of them on the following table: Object Mass (kg) Radius (km) Density (g/cm3) Jupiter Io Europa Ganymede Callisto Table 1: Chart of properties of Jupiter and the Galilean Moons Now that you are familiar with the Galilean moons, choose your favourite one for the following activities. Your Moon Activity 2: Calculate the period of your favourite moon The third Kepler’s Law involves several orbital parameters, and the periodicity of the motion (period or T term in the equations) is one of them. You will calculate the period using “Stellarium”. Open Stellarium Open the console, by pressing F12, and paste the following script on it: core.setObserverLocation("Madrid, Spain"); LandscapeMgr.setFlagLandscape(false); LandscapeMgr.setFlagAtmosphere(false); LandscapeMgr.setFlagFog(false); core.selectObjectByName("Jupiter", true); core.setMountMode("equatorial"); core.setTimeRate(3000); StelMovementMgr.setFlagTracking(true); StelMovementMgr.zoomTo(0.167, 5); Mass of Jupiter 9 CESAR Science Case Once you are done click on the play button ( ) and a figure similar to Figure 9 will be displayed Figure 9: Stellarium view, after running the script The name of the Galilean moons will be displayed. Check how your favourite moon moves around Jupiter. It is following a periodic motion! However, as you may guess the real motion is slower (indeed 3000 times slower). Slow down the motion at your convenience. Calculate how much time your moon spends in doing a complete loop around Jupiter. For this pay attention to the parameters “date” and “time” at the lower part of the display. Select one point in time and write down the value. See the evolution of the movement and note down the time when the moon is again at the same position. The difference between those 2 points is the period. Initial date (YYYY-MM-DD hh:mm:ss) Final date (YYYY-MM-DD hh:mm:ss) Calculate the time difference here Table 2: Moon period calculation Write down the result of your moon here: Period days hours Mass of Jupiter 10 CESAR Science Case Figure 10: Jupiter Moons visualization (Credit: CESAR) As shown in Figure 10, be aware that in Stellarium we are seeing Jupiter as it is seen from Earth. However, the motion of the moons is circular, but we are just watching a projection in 2 dimensions. Did you know? Jupiter has always been a very interesting astronomical object to study. Since the first observation from Galileo a lot of improvements have been achieved. Figure 11: Artist's concept of the proposed JUICE mission to the Jupiter system (Credit: Wikipedia) Several space missions have passed very close to this planet: like Pioneer 10 and 11, both Voyager 1 and 2, Galileo, Cassini-Huygens and Ulysses has made some fly-bys around Jupiter. And other missions like JUNO (from NASA) have been developed for this planet in particular. ESA is currently working in JUICE, which will be launched in 2022. Mass of Jupiter 11 CESAR Science Case Activity 3: Calculate the orbital radius of your favourite moon The orbital radius of a moon, assuming a circular movement, can be defined as the maximum distance between Jupiter and your moon. As you can see in Figure 13 , this value can be obtained by using trigonometry basis. To calculate this you will make use of Stellarium and the plugin Angle Measure. Note: Make sure the plugin “Angle Measure” is active in your configuration. Otherwise do the following: • Move your mouse to the left part of the screen • Open the configuration menu (or F2 in your keyboard) • Select Angle Measure > Load at startup • Restart Stellarium. Ready for calculating the radius? Follow the next steps to make the measurement: • Stop the motion of the moons around Jupiter by pressing in the lower menu (or K in your keyboard) • Move your mouse again to the lower menu and press (you can also press Ctrl + A) in order to enable the Angle Measuring plugin. • Click on the centre of Jupiter and later the centre of your favourite moon. WARNING: The Kepler’s Laws are just valid if the measurement is done from the centre of the astronomical objects, so be sure that you click on the centre of the moon and the centre Jupiter. Figure 12: Using Angle Measure plugin • Write down your measurement here, in the column 2 in the units given by the program. Convert these units to degrees (with decimals) and write down the distance in degrees. Note: We are considering angular distance, that is why the units are given in degrees. Mass of Jupiter 12 CESAR Science Case Maximum Distance ° ‘ ‘’ ° of your Moon to Jupiter Write your calculations here Remember: 1° = 60’ and 1’= 60’’ → 1°= 3600 ’’ Did you know? The relationship between the angular distance (휃) and the orbital distance of every moon (푅) to Jupiter, can be calculated using basic trigonometry; and lastly(푑퐽퐸) is the distance from Jupiter to the Earth, which is obtained with Stellarium. As you can see in Figure 13 we can use the definition of the sine, which states that: “in a rectangular triangle, the ratio between the length of the opposite side of an angle and the length of the hypotenuse is the sine of that angle”.
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