COMS.PERS.SOLAR SYSTEM ASTR 2 PKG
COMS.PERS.SOLAR SYSTEM ASTR 2 PKG
18th Edition
ISBN: 9781323878552
Author: Bennett
Publisher: Pearson Custom Publishing
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Chapter 1, Problem 46EAP

Driving Trips. Imagine that you could drive your car at a constant speed of 100 km/hr (62 mi/hr), even across oceans and in space. (In reality, the law of gravity would make driving through space at a constant speed all but impossible.) How long would it take to drive

a. around Earth’s equator? b. from the Sun to Earth?

c. from the Sun to Pluto? d. to Alpha Centauri?

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1. Why were the main reasons why the idea that the Earth was at the center of the universe lasted so long? 2. Discuss in 2 paragraphs the observations made by Galileo that disproved Geocentrism. Which one do you think was the most important? 3. Write down a hypothesis and observational experiment to test one of Newton’s laws of motion. EXPLAIN YOUR REASONING! 4. One of the first exoplanets discovered orbits the star 51 Pegasi with a period of just 4.2 days. 51 Pegasi is very similar to the Sun. Use Kepler’s laws to find the distance (in astronomical units) between the planet (unofficially named Bellerophon) and its star. SHOW YOUR WORK! 5.  How does halving the distance between two objects affect the gravitational force between them? 6. Suppose the Sun were somehow replaced by a star with five times as much mass. What would happen to the gravitational force between the Earth and the Sun? 7. How long would the Earth year last in this last case? (hint: Newton’s version of Kepler’s 3rd…
1. Which planetary model allows a scientist to predict the exact positions of the planets in the night sky over many years?               2. Which object orbits Earth in both the Earth – centered (geocentric) and Sun – centered (heliocentric) models of our solar system?               3. What is the actual shape of the Earth’s orbit around the Sun?
Using Kepler’s Third Law (r3 = MT2 where M is the mass of the central star) find the orbital radius in astronomical units of this planet. M = 1.5 times the mass of the sun. Remember to convert days to years using 365.25 as the length of a year in days.  Key Points to know:  - The semimajor axis of the planet in AU is r = 0.0379 AU - The  circumference of the orbit is l = 3.562 x 10^10 m  - The orbital velocity in m/s is v = 1.874 x 10^5 m/s Questions that need to be answered:  - With that orbital velocity, the radius of the orbit in meters, find the centripetal acceleration of our exoplanet:  - Knowing the acceleration that our planet experiences, calculate the force that the host star exerts on the planet:  - Knowing the force on the planet, the orbital radius, and the mass of the parent star, use the equation for gravitational force to find the mass of our planet (m2). (To get m1 in kg multiply the mass of the star in solar masses by 1.98 x 1030).

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COMS.PERS.SOLAR SYSTEM ASTR 2 PKG

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