Week 2 in Class Notes
Week 2 in Class Notes ASTR 101
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This 2 page Class Notes was uploaded by Evan Kirkpatrick on Sunday October 11, 2015. The Class Notes belongs to ASTR 101 at University of Washington taught by Ana Larson in Fall 2015. Since its upload, it has received 24 views. For similar materials see ASTRONOMY (NW,QSR) in Environmental Science at University of Washington.
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Date Created: 10/11/15
Week 2 in Class Notes Our Cosmic Address Earth Solar System Orion Arm Milky Way Local Group of Galaxies Local Supercluster of galaxies Universe The Night Sky Every star that we see in the sky is part of the Milky Way We can see 3 galaxies with the naked eye 0 1 Andromeda o 2 Large Magellanic Cloud 0 3 Small Magellanic Cloud Constellations Speci c region of the sky stars and objects placed with official borders We see different constellations throughout the year because of Earth s orbit around the Sun 0 The Sun prevents us from seeing all constellations at one time because of it s brightness Celestial Sphere Celestial Equator is right above our equatior Celestial NorthSouth Pole is right above our NorthSouth Pole The Sphere allows us to locate things around the Earth used as a map Energy Kinetic Energy12 x Mass x Velocityquot2 Gravitational Potential Energy Mass x Acceleration due to gravity x Height Thermal Energy Kinetic energy that also determines the temperature Dark matter and dark energy make up most of the universe Fission Breaking apart massive nuclei Fusion Combining atoms together to form larger elements Newton s Laws of Motion 1 Objects at Rest Stay at Rest While Objects in Motion Stay in Motion 0 Forces can push and pull and balance each other out Forces that cancel out have no effect on the objects motion 0 An object will continue to move in the same direction until a force acts on it to slow it or speed it 0 Similarly an object will remain at rest unless a force acts on it to move it 2 Force Changes an Objects Motion 0 Forces can change either the speed or the direction 0 The speed and direction for the velocity 0 Acceleration is the rate at which the velocity changes Acceleration can be positive or negative 0 Net forces cause acceleration o lnertia also affects acceleration The greater the mass the greater inertia and therefore the greater the force needs to be in order to accelerate the object 3 Whatever is Pushed Pushes Back 0 Every time one object exerts a force on another a matching force is exerted by the second object onto the rst object Exactly as strong but in the opposite direction 0 All forces come in pairs and every pair has an equal strength but opposite direction Gravity Force of gravity G x the product of the masses divided by the distance squared Force of gravity depends on the mass of the planet or object you are standing on 0 Eg Gravity is stronger on the Sun because its more massive than Ea h
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