A Sense of Proportion: Arrange the following in order of increasing length: Fill in the blanks with words that would best complete the passage. Totality a lunar eclipse one year one revolution of the Moon around Earth one saros cycle —'—'—
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- How Do We know? Why must a scientific argument dealing with some aspect of nature include all of the evidence?One way to recognize a distant planet is by its motion along its orbit. If Uranus circles the Sun in 84 years, how many arc seconds will it move in 24 hours? (For the purposes of this problem, ignore the motion of Earth.)3.) Light travels at the speed of 1.17 x 10^7 miles per minute. Pluto’s average distance from the Sun is 3,670,000,000 miles. On average, how long does it take sunlight to reach Pluto? Write your answer in scientific notation. with solution
- Part 3 1. The diameter of the Sun is 1,391,400 km. The diameter of the Moon is 3,474.8 km. Find the ratio, r= Dsa/Dsvan between the sizes. 2. From the point of view of an obs erver on Eanth (consider the Earth as a point-like object), during the eclipse, the Moon covers the Sun exactly. Sketch a picture to illustrate this fact. Use a nuler to get a straight line. Your drawing does not need to be in scale. 3. The Sun is 1 Astronomical Unit (AU) away from the Earth. Find the distance between the Earth and the Moon in AU's using the ratio of similar triangles. Show your work. DEM= AU. Convert this to kilometers. Use 1 AU = 149,600,000 km. DEM = km.1) Thinking about the Scale of the Solar System As we discuss in class, the radius of the Earth is approximately 6370 km. The Sun, on the other hand, is approximately 700,000 km in radius and located, on average, one astronomical unit (1 au=1.5x108 km) from the Earth. Imagine that you stand near Mansueto Library, at the corner of 57th and Ellis. You hold a standard desk globe, which has a diameter of 12 inches, and you want to build a model of the Sun, Earth, and their separation that keeps all sizes and lengths in proportion to one another. a) How big would the Sun be in this scale model? Give your answer in feet and meters.a. Describe the concept of “sphere of influence” and how it is estimated. b. Calculate the SOI for the Moon relative to the Earth. c. Would a single lone star have a computed sphere of influence, as defined in this class, which could be calculated? If no, why not? If yes, how would you do it?
- QUESTION 1 Estimate The Temperature For A Planet In Other Solar System (Questions 1-3) Let us assume scientists just discovered a planet orbiting a star in an extra-solar system. The star has a surface temperature Ts = 10000 Kelvins and a radius Sr = 1x109 meters. Scientists also measured the distance (D) between the star and the planet as D = 2 AU - 3.0x1011 meters. The solar power per unit area from the star's surface (Ps) can be calculated from the star's surface temperature Ts (10000 Kelvins) by the Stefen-Boltzman law Ps=0(Ts)4, where o is Stefen-Boltzman constant (5.67 x 10-8 Watt/meter2/Kelvin4). What is the solar power per unit area from the star's surface (Ps)? O Ps ~ 2.87 x 108 Watt/meter2 O Ps ~ 5.67 x 108 Watt/meter2 O O Ps ~ 2.87 x 10 Watt/meter2 Watt/meter² Ps ~ 5.67 x 10⁹ QUESTION 2 The solar power (Ps) decreases from the star's surface to the distance at the planet. Assuming the solar power per unit area at the distance of the planet as Pp, we have Pp=Ps(Sr/D)2, where…how do you compare us with people from the moon. Explain?Question 1 (Total: 30 points) a. What is a repeat ground-track orbit? b. Explain why repeat ground-track and Sun-synchronous orbits are typically used for Earth observation missions. c. The constraint for a Sun-synchronous and repeat ground-track orbit is given by T = 286, 400, where I is the orbital period in seconds, m the number of days and k the number of revolutions. Explain why this is, in fact, a constraint on the semi-major axis of the orbit.