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The History of Astronomy
The Roots of Astronomy● Already in the stone and bronze ages,
human cultures realized the cyclic nature of motions in the sky.
● Monuments dating back to ~ 3000 B.C. show alignments with astronomical significance.
● Those monuments were probably used as calendars or even to predict eclipses.
Stonehenge
Stonehenge
● Constructed 3000 – 1800 B.C. in Great Britain
● Alignments with locations of sunset, sunrise, moonset and moonrise at summer and winter solstices
● Probably used as calendar
Amazon Stonehenge
Constructed around A.D. 100 in Brazil
Other Examples around the World
Caracol (Mexico); Maya culture, approx. A.D. 1000
Ancient Greek AstronomersModels were based on unproven “first
principles”, believed to be “obvious” and were not questioned:
Geocentric “Universe”: The Earth is at the Center of the “Universe”.
“Perfect Heavens”: The motions of all celestial bodies can be described by motions involving objects of “perfect” shape, i.e., spheres or circles.
Ptolemy: Geocentric model, including epicycles
Central guiding principles:1. Imperfect, changeable Earth2. Perfect Heavens (described by spheres)
Epicyclesa small circle whose center moves around
the circumference of a larger one.
Introduced to explain retrograde (westward) motion of planets
The Copernican Revolution
Nicolaus Copernicus (1473 – 1543): Heliocentric Universe (Sun in the Center)
New (and correct) explanation for retrograde motion of the planets:
This made Ptolemy’s epicycles
unnecessary.
Retrograde (westward) motion of a
planet occurs when the
Earth passes the planet.
Described in Copernicus’ famous book “De Revolutionibus Orbium Coelestium” (“About the revolutions of celestial objects”)
Johannes Kepler (1571 – 1630)
Used the precise observational tables of
Tycho Brahe (1546 – 1601) to study planetary motion
mathematically.
Planets move around the sun on elliptical paths, with non-uniform velocities.
Found a consistent description by abandoning
both uniform motion & circular motion
Kepler’s Laws of Planetary Motion
1. The orbits of the planets are ellipses with the sun at one focus.
c
Eccentricity e = c/a
Eccentricities of Ellipses
e = 0.02 e = 0.1 e = 0.2
e = 0.4 e = 0.6
1) 2) 3)
4) 5)
Eccentricities of planetary orbits
Orbits of planets are virtually indistinguishable from circles:
Earth: e = 0.0167Most extreme example:
Pluto: e = 0.248
2nd Law: A line from a planet to the sun sweeps over equal areas in equal intervals
of time.Fa
stS
low
Animation
Autumnal Equinox (beg. of fall)
Winter solstice (beg. of winter)
Summer solstice (beg. of summer)
Vernal equinox (beg. of spring)
January
July
Fall
Winter Spring
Summer
Astronomical Units (AU)1AU = (about) 150 mil km
3rd Law: A planet’s orbital period (P) squared is proportional to its average distance from the sun (a) cubed:
Py2 = aAU
3
(Py = period in years; aAU = distance in AU)
Orbital period P known → Calculate average distance to the sun, a:
aAU = Py
2/3
Average distance to the sun, a, known → Calculate orbital period P.
Py = aAU3/2
If it takes 29.46 years for Saturn to orbit once around the sun. What is its average distance from the sun?
A. 9.54 AUB. 19.64 AUC. 29.46 AUD. 44.31 AUE. 160.55 AU
Isaac Newton (1643 - 1727)
Major achievements:
Added physics interpretations to the mathematical descriptions of astronomy by Copernicus, Galileo and Kepler
2. Discovered the three laws of motion3. Discovered the universal law of mutual
gravitation
1. Invented Calculus as a necessary tool to solve mathematical problems related to motion
Newton’s Laws of Motion (I)
1. A body continues at rest or in uniform motion in a straight line unless acted upon by some net force.
An astronaut floating in space will float forever in a straight line unless some external force is accelerating him/her.
Velocity and AccelerationAcceleration (a) is the change of a
body’s velocity (v) with time (t):a = Δv/Δt
Velocity and acceleration are directed quantities (vectors)!
a
v
Newton’s Laws of Motion (II)2. The acceleration a of
a body is inversely proportional to its mass m, directly
proportional to the net force F, and in the
same direction as the net force.
a = F/m ⬄ F = m a
Newton’s Laws of Motion (III)
3. To every action, there is an equal and opposite reaction.
The same force that is accelerating the boy forward, is accelerating the skateboard backward.
The Universal Law of Gravity
A particle attracts every other particle in the universe using a force that is directly proportional to the product of their masses and inversely proportional to the square of the distance between them.
F = - G Mmr2
(G is the Universal constant of gravity.)