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58 Cards in this Set

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equinox
day when sun stands over equator
summer solstice
day when sun is farthest north
heliocentric
sun centered model
sterllar parallax
angular shift in position due to oberservation from different points
celestial spehere
large dome containing stars
period
time for planet to circle sun
winter solstice
day when the sun is farthest south
astronomical unit
distance from Earth to Sun
retrograde motion
back and forth motion of a planet
epiccle
small circele a planet goes around to produce retrograde motion
angle of elongation
angle bettween a line from Earth and the sun and Earth and a planet
motion of sun, planets, and moon
East to west in 24 hours
West to East among stars
North to South on horizon
Law of Areas
Kepler
1st geocentric model
Plato
20+years of data collection
Brahe
Proposed equant
Ptolemy
Teachings became dogma of Catholic Church
Aristotle
1st to propose heliocentric
Aristarchus
1st to measure radius of Earth
Eratosthenes
Universal Law of Gravitation
Newton
1st saw moons of Jupiter
Galileo
Law of elliptical orbits
Kepler
tried to fit planets orbit into 5 perfect solids
Kepler
1st saw phases of Jupiter
Galileo
1st predicted radius of planetary orbit
Copernicus
1st to see sunspots
Galileo
1st predicted return of comet
Halley
Found gravitational constant
Cavendish
Gave us 3 laws of motion
Netwon
Law of areas
Kepler
Harmonic Law
Kepler
planetary motion had to be pperfect circle and constand rate
Plato
proposed eccentric
Ptolemy
1st to predict periods of veolution
copernicus
gave us epicycle
ptolemy
Tried to do away with eqant
Copernicus
1st to see mountains on the moon
Galileo
did away with epicycle
copernicus
Geocentric
Earth centered model
Ecliptic
belt of stars around equater containing zodiac signs
Vernal Equinox
March 21
Summer Solstice
June 1
Autumnal Equinox
Sept. 21
Winter solstice
Dec. 21
Eccentric
Point that was center of planets rotation, but not center of Earth
equant
Pont that could be different from eccentric, but motion of planet was constant fate from equant
epicycle
small circle the planet went around while the center of the circle followed circular path around Earth.
Law of Elliptical Orbits
Planets orbit sun in elliptical paths
Kepler's law of areas
line drawn from the sun to the planet would sweep out in equal areas at equal times. Planets move faster when closer to the sun
law of periods (harmonic Law)
period^2=k*radius^3

k=1y^2/au^3
Eccentricity
ratio of c/a=e (ellipse)
-as e approaches 0, the ellipse becomes closer to a circle
Newton's Universal law of gravitation
every two objects in the universe attract each other with a force that is directly proportional to the product of their masses and inversely proportional to the square of the distance F = G (m1*m2)/d^2
gravitational constant
6.67X10^-11
found by Cavendish
Centripetal force
force needed to keep a planet going in a circular path
Newton's first law
an object at rest or in uniform motion will remain at rest or uniform motion until some unbalanced outside force is applied to it
Newton's 2nd law
Acceleration of a body is directly proportional to the force applied to ti and inversely proportional to its mass

F=ma
Newton's 3rd law
whnever one body exerts a force on a second body, the second body exerts an equal and oppositve force on the 1st body
Perturbation
when a planet is slightly pulled out of its orbit due to another planet