CHAPTER 2:CHAPTER 2:Gravitation and the Waltz of the Planets

Historical Background Ancient Greeks Ptolemy Copernicus Galileo Brahe Kepler Newton

Two Views of the Universe Geocentric model (earth-centered) Heliocentric model (sun-centered)

Ancient Greeks

Geocentric Model of the Universe Stationary Earth All other objects circle the Earth. Universe consisted of stars, six planets

(none beyond Saturn), the Sun and Moon. Stars were fixed onto a crystal sphere

that surrounded the Earth. Since the sphere rotated around the

Earth, so did the stars.

Geocentric Model of the Universe Planets shift slowly eastward relative

to the fixed stars. Planets were also observed to

occasionally move “backwards” (east to west or westward with respect to the background stars)

This was called retrograde motion. This was a problem to explain.

As the Earth rotates during the night (diurnal motion) the planet appears to move from east to west.

Looking South

From night to night, the planets appear to move from west to east relative to the background stars (direct motion).

The ancient Greeks knew that the planets slowly shifted relative to the fixed stars in the constellations.

Looking South

But sometimes, the planet would slow down, stop and reverse its motion from east to west relative to the background stars (retrograde motion).

Looking South

Geocentric Model

Early models of the universe attempted to explain the Early models of the universe attempted to explain the motion of the five visible planets against the motion of the five visible planets against the background of background of ““fixedfixed”” stars. The main problem was stars. The main problem was that the planets do not move uniformly against the that the planets do not move uniformly against the background of stars, but instead appear to stop, move background of stars, but instead appear to stop, move backward, then move forward again. This backward backward, then move forward again. This backward motion is referred to as motion is referred to as retrograde retrograde motion.motion.

Ptolemy’s Role in the Geocentric Model

1st Century

Geocentric Model of the Universe Hipparcus was first to use epicycles to

address the problem of retrograde motion of the planets.

Ptolemy expanded upon this. Ptolemy determined that retrograde

motion of planets could be described by using deferents (orbital path around Earth) and epicycles (planet’s orbital path around the deferent).

All orbits, deferents and epicycles were in perfect circles.

Epicycles and Deferents

Ptolemy explained this motion using a Ptolemy explained this motion using a geocentric geocentric (Earth-(Earth-centered) model of the solar system in which the planets centered) model of the solar system in which the planets orbited the Earth indirectly, by moving on epicycles orbited the Earth indirectly, by moving on epicycles which in turn orbited the Earth.which in turn orbited the Earth.

Ptolemy expanded upon Hipparcus’s work

Epicycles and Deferents

Stop the madness!

Occam’s Razor: the best explanation is the simplest

Copernicus and the Heliocentric Model

1500’s

Copernicus’s Heliocentric Model Sun placed at the center of the solar

system. Planets placed in proper order away from

the Sun. Synodic and sidereal periods for each

planet’s orbit were measured. Copernicus still assumed perfect circular

orbits for planets. This was a problem.

Nicolaus Copernicus in the 16Nicolaus Copernicus in the 16thth century century developed the first heliocentricdeveloped the first heliocentric (sun-centered) (sun-centered) model of the solar system. In this model, the model of the solar system. In this model, the retrograde motion of Mars is seen when the retrograde motion of Mars is seen when the Earth passes Mars in its orbit around the Sun. Earth passes Mars in its orbit around the Sun. Lack of an explanation for this motion was a Lack of an explanation for this motion was a significant failing of Copernicussignificant failing of Copernicus’’ model. model.

FYI:

Aristarchus in 6th century B.C. first suggested that the Sun was fixed and the Earth moved around the Sun in a circle.

Heliocentric vs. Geocentric Model

Ptolemy’s geocentric model failed to reproduce observed planetary motions.

heliocentricgeocentric

Tycho Brahe and Kepler—True Planetary Motion

Late 1500’s to 1600

Tycho Brahe’s observations Set up an observatory called Uraniborg in

1576 (later, he built another observatory called Stjerneborg).

He accurately measured the position and angle of stars and planets without a telescope (it had not been invented).

Huge collection of data. Brahe invited Johannes Kepler to join him

in at Uraniborg in 1600.

After Tycho BraheAfter Tycho Brahe’’s death, s death, Johannes Kepler (pictured Johannes Kepler (pictured here with Tycho in the here with Tycho in the background) used Tychobackground) used Tycho’’s s observations to deduce the observations to deduce the three laws of planetary three laws of planetary motion.motion.

Kepler’s Breakthrough Brahe asked Johannes Kepler to join

him in Denmark in 1600. Kepler used Brahe’s data to make

highly precise calculations of planetary orbits.

Accuracy of orbits matched only if orbits were considered less than perfect circles (an ellipse).

Kepler’s Breakthrough Kepler developed three laws that

could be used to describe planetary motion.

Laws are based upon the understanding of the ellipse.

LAW #1. The orbit of a planet around the Sun is an ellipse LAW #1. The orbit of a planet around the Sun is an ellipse with the Sun at one focus.with the Sun at one focus.

Semi-major axis is half the major axis

LAW #2: A line joining the planet and the Sun sweeps out LAW #2: A line joining the planet and the Sun sweeps out equal areas in equal intervals of time.equal areas in equal intervals of time.

Planet moves Planet moves faster in its orbit faster in its orbit when closer to the when closer to the Sun.Sun.

Planet moves Planet moves slower in its orbit slower in its orbit when farther away when farther away from the Sun.from the Sun.

LAW #3: The square of a planetLAW #3: The square of a planet’’s sidereal period around the Sun s sidereal period around the Sun is directly proportional to the cube of its semi-major axis.is directly proportional to the cube of its semi-major axis.

This law relates the amount of time for the planet to complete one orbit around the Sun to the planet’s average distance from the Sun.

If we measure the orbital periods (P) in years and distances (a) in astronomical units, then the law mathematically can be written as P2 = a3.

The amount of elongation in a planetThe amount of elongation in a planet’’s orbit is defined as s orbit is defined as its its orbital eccentricity.orbital eccentricity. An orbital eccentricity of 0 is a An orbital eccentricity of 0 is a perfect circle while an eccentricity close to 1.0 is nearly a perfect circle while an eccentricity close to 1.0 is nearly a straight line. straight line.

In an elliptical orbit, the distance from a planet to the In an elliptical orbit, the distance from a planet to the Sun varies. The point in a planetSun varies. The point in a planet’’s orbit closest to the s orbit closest to the Sun is called Sun is called perihelion, perihelion, and the point farthest from the and the point farthest from the Sun is called Sun is called aphelion.aphelion.

Galileo and the Telescope

1609 -1610

Galileo was the first to use a telescope to Galileo was the first to use a telescope to examine celestial objects. His examine celestial objects. His discoveries supported a heliocentric discoveries supported a heliocentric model of the solar system.model of the solar system.

1. Galileo discovered that Venus, like the Moon, undergoes a series of phases as seen from Earth. In the Ptolemaic (geocentric) model, Venus would be seen in only new or crescent phases. However, as Galileo observed, Venus is seen in all phases, which agrees with the Copernican model as shown.

Phases of Venus

2. Galileo also discovered moons in orbit around the planet Jupiter. He concluded that they are orbiting Jupiter because they move across from one side of the planet to the other This was further evidence that the Earth was not the center of the universe.

Moons of Jupiter

Galileo’s Contributions 3.      Imperfections on the Moon’s

surface: The Moon’s surface was irregular and crater-filled

4.       Dark spots on the Sun: The Sun was observed to have dark spots

Galileo’s Contributions Galileo’s observations began to

erode the notion of celestial perfection and provided support for the heliocentric view of the universe.

Isaac Newton formulated three laws to Isaac Newton formulated three laws to describe the fundamental properties of describe the fundamental properties of physical reality.physical reality.

NEWTONNEWTON’’S THREE LAWS OF MOTIONS THREE LAWS OF MOTION

LAW #1: A body remains at rest or moves LAW #1: A body remains at rest or moves in a straight line at constant speed unless in a straight line at constant speed unless acted upon by a net outside force.acted upon by a net outside force.

LAW #2: The acceleration of an object is LAW #2: The acceleration of an object is proportional to the force acting on it.proportional to the force acting on it.

LAW #3: Whenever one body exerts a LAW #3: Whenever one body exerts a force on a second body, the second body force on a second body, the second body exerts an equal and opposite force on the exerts an equal and opposite force on the first body.first body.

Newton also discovered that gravity, the force that Newton also discovered that gravity, the force that causes objects to fall to the ground on Earth, is the causes objects to fall to the ground on Earth, is the same force that keeps the Moon in its orbit around same force that keeps the Moon in its orbit around the Earth. the Earth.

NEWTONNEWTON’’S LAW OF UNIVERSAL GRAVITATIONS LAW OF UNIVERSAL GRAVITATION

Two objects 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 between them.

With his laws, Newton was able to derive Kepler’s three laws, as well as predict other possible orbits.

NewtonNewton’’s laws were applied to other objects in our s laws were applied to other objects in our solar system.solar system.

Using Newton’s methods, Edmund Halley worked out the details of a comet’s orbit and predicted its return.

Deviations from Newton’s Laws in the orbit of the planet Uranus led to the discovery of the eighth planet, Neptune.

We define special positions of the planets in their orbits depending We define special positions of the planets in their orbits depending where they appear in our sky. For example, while at a conjunction,where they appear in our sky. For example, while at a conjunction, a a planet will appear in the same part of the sky as the Sun, while at planet will appear in the same part of the sky as the Sun, while at opposition,opposition, a planet will appear opposite the Sun in our sky.a planet will appear opposite the Sun in our sky.

However, the cycle of these positions (a synodic However, the cycle of these positions (a synodic period) is different from the actual orbital period of the period) is different from the actual orbital period of the planet around the Sun (a sidereal period) because planet around the Sun (a sidereal period) because both the Earth and the planet orbit around the Sun.both the Earth and the planet orbit around the Sun.

Measuring Distances Parallax view

When a new “star” appeared in the sky during the 16th century, a Danish astronomer named Tycho Brahe reasoned that the distance of the object may be determined by measuring the amount of parallax.

The apparent change in the location of an object due to the difference in location of the observer is called parallax.

Because the parallax of the “star” was too small to measure, Tycho knew that it had to be among the other stars, thus disproving the ancient belief that the “heavens” were fixed and unchangeable.

Heliocentric Model Who is responsible? Evidence? Lacking evidence? What did Galileo discover? What are planetary configurations?

WHAT DID YOU THINK? What makes a theory scientific? If it makes predictions that can be

objectively tested and potentially disproved.

What is the shape of the Earth’s orbit around the Sun?

Elliptical Do the planets orbit the Sun at constant

speeds? The closer a planet is to the Sun in its orbit,

the faster it is moving. It moves fastest at perihelion and slowest at aphelion.

WHAT DID YOU THINK? Do all the planets orbit the Sun at the same

speed? No. A planet’s speed depends on its average

distance from the Sun. How much force does it take to keep an object

moving in a straight line at a constant speed? Unless an object is subject to an outside force, it

takes no force at all to keep it moving in a straight line at a constant speed.

How does an object’s mass differ when measured on the Earth and on the Moon?

Its mass remains constant.

accelerationangular momentumaphelionastronomical unitconfiguration (of a planet)conjunctionconservation of angular

momentumcosmologyellipseelongationfocus (of an ellipse)forceGalilean moons (satellites)gravityheliocentric cosmology

hyperbolainferior conjunctionKepler’s lawskinetic energylaw of equal areaslaw of inertialight-yearmassmodelmomentumNewton’s laws of motionOccam’s razoroppositionparabolaparallaxparsec

perihelionphysicspotential energyretrograde motionscientific methodscientific theorysemimajor axis (of an ellipse)sidereal periodsuperior conjunctionsynodic perioduniversal constant of gravitationuniversal law of gravitationvelocityweightwork

Key Terms

WHAT DO YOU THINK? What is the shape of the Earth’s orbit around

the Sun? Do the planets orbit the Sun at constant

speeds? Do all the planets orbit the Sun at the same

speed? How much force does it take to keep an

object moving in a straight line at a constant speed?

How does an object’s mass differ when measured on the Earth and on the Moon?

.Compare and contrast the Ptolemaic and Copernican cosmologies by explaining a variety of naked-eye observations, using both models.

2. State Kepler’s three laws of planetary motion; describe the geometric content and observational consequences of each.

3. List Galileo’s telescopic observations and explain the success or failure of Ptolemaic and Copernican models in accounting for them.

4. State and identify examples of Newton’s three laws of motion.

5. State Newton’s law of universal gravitation; identify the characteristics of this law that explain Kepler’s laws in terms of Newton’s laws.

1.      How do we interpret the history of the geocentric and heliocentric views of the universe?

2.      How do Kepler’s laws describe planetary motion?

3.      How are Newton’s laws of motion, Newton’s law of gravitation and Kepler’s laws related?

How do the planets move with respect to the Earth and the Sun

1. What is the shape of the Earth’s orbit around the Sun?

2. Do planets orbit the Sun at constant speeds?

3. Do planets orbit the Sun at the same speed?4. How much force does it take to keep an

object moving in a straight line at a constant speed?

5. What is the difference between heliocentric and geocentric cosmology?

1. What are the contributions to astronomy made by the following individuals: Ancient greeks, Ptolemy, Copernicus, Galileo, Brahe, Newton, Kepler?

2. How do Kepler’s laws describe planetary motion?

3. What is an ellipse?4. Does Venus show phases just like the

Moon?5. How to the planets orbit the Sun?

You will discover… clues suggesting that Earth is not the center of

the universe the scientific revolution that dethroned Earth

from its location at the center of the universe Copernicus’s argument that the planets orbit

the Sun why the direction of motion of the planets on

the celestial sphere sometimes appears to change

that Kepler’s determination of the shapes of planetary orbits depended on the careful observations of his mentor, Tycho Brahe

how Isaac Newton formulated an equation to describe the force of gravity

how Isaac Newton explained why the planets and moons remain in orbit