Download - Ancient Astronomy
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Ancient Astronomy
Neolithic Astronomy
Stonehenge
~ 2800 – 1700 BCE
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The Americas
Machu Picchu – the Intihuatana or “hitching post of the sun”
Several of the major cultures had complex structures that reveal astronomical alignments
Marked solstices, equinoxes, and positions of the Moon.
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The Caracol at Chitzen Itza, Yucatan ~ 800 AD
Venus was the ‘Great or Ancient Star”. Observations from slits in circular structure used to record times of its rising and setting. Measurements of Venus and moon used to establish a calendar and for timekeeping.
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N. America – Medicine Wheels in western plains
Stone alignments in a spoked wheel pattern some with large cairns that marked sight linesAll are on high places with a clear view of the horizon.
Medicine Wheel in Big Horn Mtns, Wyoming
Date from ~ 1400 - 1700
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Geocentric or Ptolemaic modelProblem – apparent backward motions of planets -- retrograde
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The Heliocentric Model
Copernicus 1473 - 1543
Kept circular orbits and epicycles, explained retrograde motion
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Galileo 1564 – 1642
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Galileo’s famous observations with the telescope
Surface of the Moon – mountains, craters
Phases of Venus –
Saturn had “ears”
4 moons of Jupiter
Milky Way made of 1000’s of stars
Sun was blemished
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Galileo’s 3 decisive discoveries for Heliocentric model : 1. Surface features on the Moon 2. Jupiter’s moons and motions 3. “Full” phases of Venus
None of these made sense in geocentric model, but they were all perfectly OK in Copernicus’ universe. The phases of Venus are especially decisive.
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Tycho Brahe 1546 – 1601
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Brahe couldn’t measure stellar parallax and therefore couldn’t confirm Copernican model -- proposed his own
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Thomas Digges – English mathematician, astronomer
1546 – 1595
Contemporary with Brahe and Galileo, but his model goes a step further
"This orb of stars fixed infinitely up extends itself in altitude spherically, and therefore immovable the palace of felicity garnished with perpetual shining glorious lights innumerable, far excelling over [the] sun both in quantity and quality the very court of celestial angels, devoid of grief and replenished with perfect endless joy, the habitacle for the elect."
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Johannes Kepler 1571-- 1630
The Astronomical Unit ( 1 AU)
distance Earth to the Sun
93 x 106 mi , 150 x 106 km
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Kepler’s 3 laws of planetary motion
1. The orbits of the planets are ellipses with the Sun at one focus
2. The line joining the planet and the Sun sweeps out equal areas in equal times.
3. Period of revolution proportional to distance from Sun
If a = average distance from the Sun and P = orbital period, then P 2 = (constant) x a 3
If P in years, a in astronomical units
then P 2 = a 3
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Kepler’s third law -- the numbers
a (AU) P (yr) a 3 P 2
MERCURY 0.387 0.241 0.058 0.058 VENUS 0.723 0.615 0.378 0.378EARTH 1.000 1.000 1.00 1.00MARS 1.524 1.881 3.54 3.54 JUPITER 5.203 11.86 141 141SATURN 9.54 29.46 868 868
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Isaac Newton 1642 -- 1727
Astronomer, mathematician, physicist – father of physics, mechanics
Laws of Motion and Law of Gravity
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The 3 Laws of Motion and the Law of Gravity
Some basic concepts:
Speed – how fast an object is moving mi/hr, km/s
Velocity -- vector – speed + direction
Acceleration – rate of change in velocity
Inertia – property of an object resists change in state of rest or motion
1st Law -- An object remains at rest or in motion (in a straight line) unless
acted upon by an outside force
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2nd Law -- The acceleration of an object is directly proportional to the force
acting on it.
F = ma Defines: Force
Mass (m) - total amount of material in an object
weight depends on the force of gravity on an object with mass m
3rd Law -- (Law of Reaction) Whenever a force is exerted on an object there
is an equal and opposite reaction
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Law of Gravity -- the force of attraction between two objects is directly
proportional to their masses and inversely proportional to the
square of the distance between them
( attractive force between M and m )
FGrav = G x M x m / (distance) 2 .
Laws of Motion + Gravity explained Kepler’s Laws
Newton’s form of Kepler’s 3rd law:
P2 = 4 2/G x a3/ (M1 + M2)
Why the difference ?
Orbital Motion is due to inertia plus gravity – the force of acceleration towards
the center -- centripetal acceleration