Astronomy
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| Kepler's 1st law of Planetary Motion | The orbit of each planet about the Sun is an ellipse with the Sun at one focus
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| Newton | Built the first reflecting telescope (1668)
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| Copernicus | Published heliocentric theory of the Universe (1543)
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| Galileo | Used telescope for astronomical purposes and discovers 4 Jovian moons, Moon's craters, and Milky Way Galaxy (1609)
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| Ptolemy | Suggested geocentric theory of the universe in work Mathematike Syntaxis (140 BC)
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| Brahe | Discovered a supernova in the constellation Cassiopeia (1572)
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| Aristarchus | Suggested the Earth revolves around the Sun. He provided the first estimate of Earth-Sun distance (280 BC)
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| Eratosthenes | Measured the circumference of the Earth with surprising accuracy (240 BC)
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| Hipparchus | Developed first accurate star map and star catalogue with over 850 bright stars (130 BC)
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| First Solar/Lunar calendars | 2000 BC in Egypt and Mesopotamia
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| Julian Calendar | Purely solar calendar implemented in the Roman Empire (45 BC)
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| Hans Lippershey | Spectacle maker invents telescope (1608)
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| Kepler | Created the 3 laws of Planetary Motion (1609 - 1619)
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| Kepler's 2nd law of Planetary Motion | As a planet moves around its orbit, it sweeps out equal areas in equal times. This tells us that a planet moves faster when it is closer to the Sun (near perihelion) than when it is farther from the Sun (near aphelion) in its orbit.
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| Newton's Laws | 3 Laws of Motion and the Universal law of gravitation
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| Newton's Laws of Motion | 1) In the absence of a net force, an object moves with constant velocity
2) a net force affects an object's motion. Force = rate of change in momentum or force = mass X acceleration
3) For any force, there is always an equal and opposite reactive force.
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| Newton's Universal law of Gravitation | The force of gravity (Fg) between two objects given by the formula Fg = G(M1M2/d2)
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| Drake Equation | Lays out the factors that play a role in determining the number of communicating civilizations in our galaxy.
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| Circles within circles | Ancient Greek theory that the earth was the center of the Universe and all planets moved in perfect circles around Earth.
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| Heliocentric | Belief that the sun is the center of the Universe
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| Geocentric | Ancient belief that the Earth is the center of the Universe
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| Conservation of energy | Energy (including mass-energy) can be neither created nor destroyed, but can only change from one form to another
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| Conservation of momentum | In the absence of net force, the total momentum of a system remains constant
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| Conservation of angular momentum | in the absence of net torque (twisting force), the total angular moment of a system remains constant
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| Azimuth | Direction around the horizon from due north, measured clockwise in degrees
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| Astronomy | The study of the Universe and movement of the planets
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| Astrology | The study of the movement of the stars and how their alignment affects people's lives
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| Stars in Milky Way | 100 Billion
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| Stars in the entire Universe | 100 Billion X 100 Billion = 10,000,000,000,000,000,000,000 or 10^22
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| Speed of Light | 300,000 km per sec
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| Size of the Earth | Earth = tip of a ballpoint pen
Sun = size of a grapefruit
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| Distance to the Sun | 1 AU or 150,000,000 km
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| Distance to the moon | 4 days from the earth
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| Age of the Solar System | 13.7 Billion Years
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| Ecliptic | Apparent movement of the sun and stars across the sky
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| Zenith | 90 degrees above the horizon (straight up)
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| Azimuth | left to right direction
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| Mass | amount of particles in a given space
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| Acceleration due to gravity | The acceleration of a falling object which is designated by g = 9.8 m/s squared
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| Energy | what makes matter move; kinetic, potential, radiative
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| Astronimical Units (AU) | The average distance (semimajor axis) of the Earth from the Sun which is about 150 million km
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| Light Year | Distance light travels in one year which is 9.45 trillion km (9.46 x 10^14) which = 300,000 km/sec
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| Rotation | The spinning of an object around its axis
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| Revolution | The orbital motion of one object around another
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