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Measuring the Universe: Earth PowerPoint PPT Presentation

Measuring the Universe: Earth Eratosthenes (about 200 BC): Sun overhead at Syene on summer solstice Sun 7 º from zenith at Alexandria on same day SO: Alexandria is 7º in latitude from Syene In terms of fractions of a circle: Measuring the Universe: Distances to Planets

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Measuring the Universe: Earth

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Measuring the universe earth l.jpg

Measuring the Universe: Earth

Eratosthenes (about 200 BC):

  • Sun overhead at Syene on summer solstice

  • Sun 7º from zenith at Alexandria on same day

    SO: Alexandria is 7º in latitude from Syene

    In terms of fractions of a circle:


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Measuring the Universe: Distances to Planets

Distances to planets and Sun helped settle whether Earth or Sun was at the center of everything…

Ancient people attempted measurements, but techniques weren’t accurate enough


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Planet Motions Across Sky

  • planets appear to circle Earth once a day

  • BUT planets move compared to stars over many days

  • planets stay near ecliptic

     ecliptic goes through zodiac constellations


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“Inferior Planets”: Mercury, Venus

VENUS

VENUS

  • always near Sun in sky

  • best seen just before sunrise or just after sunset

  • never seen at midnight

MERCURY

MERCURY

LOOKING WEST AT SUNSET

LOOKING EAST AT SUNRISE


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“Superior Planets”: Mars, Jupiter, Saturn

  • sometimes seen high overhead at midnight

  • usually move W to E relative to stars: “direct motion”

  • sometimes move E to W relative to stars: “retrograde motion”

Mars in direct motion (compared to stars)

E

W

Mars in retrograde motion


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Thought Question:

At roughly what time would the planet at position 5 be highest above the horizon? (Remember that Earth rotates counterclockwise from this point of view.)

  • 3 am

  • 9 am

  • 3 pm

  • 9 pm

  • It is not possible to tell from the diagram


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Thought Question:

Where would planet A be seen in the sky from Earth at sunset?

A


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Competing Ideas about the Universe

Geocentric Model

(Claudius Ptolemy, around 140 AD)

All planets move on epicycles (circular paths) that circle Earth

  • epicycles of inferior planets attach to a line between Earth and Sun

  • epicycles of superior planets circle Earth independently


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Competing Ideas about the Universe

Epicycles are needed to create retrograde motions of planets


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Retrograde Motion

 happens when Earth catches and passes a superior planet


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Thought Question:

Where would you look to see a planet rise when it is in retrograde motion?

  • near the eastern horizon

  • near the western horizon


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Thought Question:

If you lived on the planet Mars and you monitored Earth’s position in the sky over the course of several years, what would see?

  • Earth always moves from east to west relative to the stars.

  • Earth always moves from west to east relative to the stars.

  • Earth usually moves from west to east relative to the stars, but occasionally undergoes retrograde motion (east to west).

  • Earth is always fairly close to the Sun in the sky, and is most easily visible before sunrise or after sunset.


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Measuring the Universe: Inferior Planets

Nicolaus Copernicus (around 1530 AD)

 maximum elongation (e): largest angle between planet and Sun

 used to determine planet’s distance from Sun:

dp

e

d


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Satellite Collision


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Kepler’s Laws of Planetary Motion

Discovered by trial and error…

Kepler’s First Law: (SHAPES OF ORBITS)

All planet orbits are ellipses with Sun at one focus

eccentricity

flashlet

applet


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Eclipses

Solar eclipses can be either total or “annular”…

the Moon’s distance from Earth changes…


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Ellipses

semi-major axis (a): half length of long side

 average distance from Sun

eccentricity (e):

center

Sun

c

a

rP

rA

aphelion: farthest point from Sun

perihelion: closest approach to Sun

SPECIAL CASE: CIRCLE

semi-major axis (a) equals radius

Sun

a


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TOP VIEW:

Ellipses

Sun

Orbits are flat (they can fit in a flat plane)

BUT

They are usually tilted relative to each other…

inclination (i): angle between Earth’s and object’s orbit planes

rP

rA

SIDE VIEW:

Sun

Inclination i

Earth orbit


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Kepler’s Laws of Planetary Motion

  • Kepler’s Second Law: (SPEED DURING ORBIT)

    A line connecting Sun and planet sweeps out equal areas in equal times.

A1

flashlet

A2

CLOSER TO SUN  GREATER SPEED

applet


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Comets

Orbit


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Kepler’s Laws of Planetary Motion

(COMPARING PLANETS)

  • Kepler’s Third Law:

    P: orbital period of planet (sidereal period)

    a: planet’s average distance from Sun (semi-major axis)

Sun

applet

a

1 AU (Astronomical Unit) is Earth’s average distance from Sun

1 AU = 1.5  1011 m

applet

applet - defunct


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Thought Questions:

NASA wants to launch a spacecraft to go out to the planet Mars (without stopping there), and then come back. If the spacecraft follows the orbit below (dotted line),

  • What is the semi-major axis of the orbit?

  • How long would it take to get to Mars from Earth?

1 AU

1.5 AU


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Thought Question:

If it takes Eris 557 years to orbit the Sun, what is its average distance from the Sun?


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Kepler’s Third Law Examples

  • Jupiter:

  • Eris:

  • Sedna:


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Thought Question:

The asteroid Apophis has an orbit with the following characteristics:

  • semi-major axis: a = 0.922 AU

  • orbit period: P = 0.89 yr

  • eccentricity: e = 0.191

  • inclination: i = 3.3º

    If Earth’s orbit has a semi-major axis of 1 AU and Venus has a semi-major axis of 0.723 AU, does Apophis’ orbit cross the planet orbits?

  • Apophis always stays between Earth’s and Venus’ orbits.

  • Apophis goes outside Earth’s orbit and inside Venus’ orbit.

  • Apophis goes outside Earth’s orbit.

  • Apophis goes inside Venus’ orbit.


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Apophis – Killer Asteroid?

  • asteroid about 350 m across

  • close approach to Earth in 2029


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Measuring the Universe: Problems

  • both Earth and other planets are moving

    SO…

  • how do you determine when a planet comes back to the same place in its orbit?


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Orbit and Synodic Periods

Sidereal (orbit) periods (Porb):

time for a planet to make exactly one orbit around Sun

  • only Earth’s is directly measurable

SUN

Synodic period (Psyn) :

time between “line-ups” of Earth, Sun, and planet

  • measurable from Earth


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Periods and Angular Speeds

From Sun’s point of view:

Fast planet orbits in timePfast:

  • moves W to E with angular speed:

    Slow planet orbits in timePslow:

  • moves W to E with angular speed:

    LINE-UPS:

  • Because both move in same direction, it takes longer for fast planet to “lap” slow one (travels an extra 360º in time Pline-up)

  • rate:


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Thought Question:

It takes Earth, Venus, and Sun 584 days to go between line-ups. What is Venus’ orbit period?

(Hint: Which planet is the fast one, and which is the slow one?)


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Parallax

Two observers on Earth see planets in slightly different positions in sky (compared to stars)

  • the bigger the angle, the closer the planet must be

angle a

… this is the same idea behind your two eyes


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The “Asteroid Tugboat”

  • spacecraft lands and fires rocket to push asteroid

  • if asteroid is spinning, spacecraft must land at a “pole”

  • less effort required if done farther in advance

  • What direction will the asteroid go?


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VELOCITY

Newton’s Laws of Motion

  • speed: how fast an object’s position changes

    measured by speedometers, radar guns

  • velocity: speed and direction of travel

    measured by weather vanes

  • First Law: An object will maintain a constant velocity if there is no net force acting on it.


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Newton’s Laws of Motion

  • acceleration: how fast velocity changes

    3 ways to accelerate a car:

  • GAS PEDAL (change speed)

  • BRAKE PEDAL

  • STEERING WHEEL (change direction)

  • force: strength and direction of a push or pull

    any effort that can cause acceleration

  • Second Law: For an unbalanced force,

    a: acceleration (units: m / s2)

    m: mass(units: kg)

    F: force (units: Newton = kg · m / s2)


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Thought Question:

The pictures below show strobe-light pictures of trucks at different times.

  • Which of the trucks is showing acceleration? (There may be more than one.)

  • For the accelerating trucks, what direction is the net force on the truck pointing?

POSITION (m)


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Earth Acceleration due to Gravity (g = 9.8 m/s2)

DISTANCE FALLEN

TIME

SPEED

0 s

0 m/s

0 m

SPEED

1 s

9.8 m/s

4.9 m

2 s

19.6 m/s

19.6 m

TIME

DISTANCE

3 s

29.4 m/s

44.1 m

TIME


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Orbits are Curved Paths

Newton’s First Law says: If object is traveling on a curved path, there MUST BE an unbalanced force.

FORCE

TOP VIEW:

VELOCITY

VELOCITY

FORCE

(friction between tires and road)

(gravity)

Newton’s Second Law says: object accelerates (turns) in direction of unbalanced force

 force is NOT pushing planet forward

 force IS pulling toward inside of orbit (toward Sun)


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Thought Question:

The picture below shows the velocity of a planet at different times in its orbit (larger arrow means larger speed).

B

Draw the direction of the force on the planet at the different positions shown

C


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PLANET’S VELOCITY

Ellipse Orbit:

SUN’S FORCE TURNS AND SLOWS PLANET

PLANET’S VELOCITY

SUN’S FORCE TURNS AND SPEEDS PLANET

SUN’S FORCE JUST TURNS PLANET


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Newton’s Thought Experiment

Fire cannonballs from tall mountain at different speeds:

low speed: crash into surface

medium speed: circular orbit

high speed: ellipse orbit (cannonball gets farther from Earth)


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Thought Question:

A ball is attached to a string and swung in a circular path above my head. At the point shown below, I suddenly release the string. If this is viewed from directly above, which of the paths below would the ball most closely follow when released?

VIEW FROM ABOVE:


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USA

Newton’s Laws of Motion

  • Third Law: When one object exerts a force on a second one, the second object exerts an equal and opposite force back on the first.

EXAMPLES:

GAS FORCE ON ROCKET

ROCKET’S FORCE ON GAS

SKATER FORCES ON EACH OTHER

ICE


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Thought Questions:

A compact car and a large truck collide head-on and stick together.

  • Which one feels the largest force during the collision?

  • Which one experiences the largest acceleration?

  • The car.

  • The truck.

  • Both experience the same amount.

  • You can’t tell without knowing how fast they were moving before the collision.


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The “Gravity Tractor”

  • satellite uses rocket to hover near asteroid

  • gravity of satellite changes path of asteroid

  • less effort required if done farther in advance

  • What direction will the satellite pull the asteroid?


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Universal Gravitation

  • Fg: force

  • m1, m2: masses

  • d: distance between centers of objects

  • G: universal gravitational constant

  • attractive force: always pulls masses together

  • equal strength forces pull on both masses


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Acceleration of Gravity

Galileo’s Experiment:

Two different masses dropped at same time hit ground at same time…

implies equal acceleration

At Earth’s surface, force is

which creates an acceleration:

that doesn’t depend on the mass of the object!


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Acceleration Needed for a Curved Path


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Circular Orbit Speed


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General Form of Kepler’s Third Law

  • Mtotal: total amount of mass involved (example: star and planet)

  • applies to any elliptical orbit

  • appliesto any masses (Sun and planet; Earth and satellite; Jupiter and a moon;…)

  • AN ASTRONOMER’S MAIN WAY TO DETERMINE MASS!

  • …just need orbital period and average orbital distance


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Center of Mass

center of mass


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The Center of the Milky Way

Stars appear to be orbiting something dark…

and about 4 million times the Sun’s mass!


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Measuring New Planets

Newton’s Third Law: star moves slightly as planet orbits

If we can figure out roughly how massive the star is, we can figure out how big the planet’s orbit is…

PLANET’S FORCE ON STAR

STAR’S FORCE ON PLANET


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Thought Question

Suppose you found a star with the same mass as the Sun moving back and forth with a period of 16 months—what could you conclude?

  • It has a planet orbiting at less than 1 AU.

  • It has a planet orbiting at greater than 1 AU.

  • It has a planet orbiting at exactly 1 AU.

  • It has a planet, but we do not have enough information to know its orbital distance.


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Thought Question:

A new planet is discovered orbiting a star that is 4 times as massive as the Sun. Astronomers find that it takes 0.5 yr to make one orbit. What does this say about the planet’s orbit?

  • The planet orbits 1 AU from its star.

  • The planet orbits more than 1 AU from its star.

  • The planet orbits less than 1 AU from its star.

  • It isn’t possible to tell how big the planet’s orbit is.


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Conservation Laws

Specific combinations of variables have the property of keeping the SAME TOTAL VALUE before and after collisions, etc.

MOMENTUM: mass  velocity

Forces change momentum, but “equal and opposite forces” ensures total momentum remains constant


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Angular Momentum

The larger the angular momentum, the harder it is to stop its spinning or revolving

  • m: mass of object

  • v: speed of rotation or revolution (perpendicular to line from center to object)

  • r: distance from center of motion

CONSERVATION OF ANGULAR MOMENTUM: amount of angular momentum does not change unless a twisting force acts on the object


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Thought Question:

Your daring professor sits in the “CHAIR OF DEATH” and starts rotating with his arms outstretched. If he pulls his arms in toward his body, and then moves them back to their original position, what will happen?

  • He will be spinning noticeably slower at the end.

  • He will be spinning at about the same speed at the end.

  • He will be spinning noticeably faster at the end.

  • Something horrible will happen…


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Thought Question:

If your daring professor sits in the “CHAIR OF DEATH” and starts rotating, what will happen if he moves his arms up and down parallel to his spin axis?

  • He will start to spin much slower.

  • He will keep spinning at the same speed.

  • He will start to spin much faster.

  • Something horrible will happen…


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Conservation of Angular Momentum

Sun


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Energy

The ability to get masses to move…

  • Metric unit: Joule (J)

  • English unit: Calorie

  • energy to pick a burger off floor (move it up by 1 m): 1 J

  • energy from eating candy bar: 106 J

  • energy released by H bomb: 5  1015 J

  • energy released by Sun each second: 4  1026 J


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Types of Energy: Kinetic Energy

  • kinetic energy: energy of motion

  • thermal energy (heat): kinetic energy involving random motions of atoms and other particles

    higher temperature  more thermal energy

EXAMPLE: GAS IN A BOX


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Thought Question:

How fast does a 1010 kg asteroid have to be traveling to have a kinetic energy equal to an H bomb (5  1015 J)?


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Types of Energy: Potential Energy

  • potential energy: energy of position – a kind of “stored” energy

    The farther an object falls, the more “stored” energy is turned into kinetic energy:

POTENTIAL ENERGY DECREASES AND…

BECOMES KINETIC ENERGY


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Energy

CONSERVATION OF ENERGY: energy can be transferred from object to object, or converted from one form to another, but never destroyed


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USA

USA

Thought Question:

A spacecraft is moving away from the Sun without firing its engines. Which of the following describes what will happen to…

  • the spacecraft’s kinetic energy?

  • the spacecraft’s potential energy?

  • the spacecraft’s total energy?


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Bound and Unbound Orbits

  • BOUND ORBIT – object does not have enough kinetic energy to escape

  • UNBOUND ORBIT – object can eventually reach d = ∞

miniature golf analogy: imagine the Sun at bottom of a well, and object rolling along the sides


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“Gravitational Well”

Imagine objects rolling on a surface that is dented by the gravity of large masses:


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Bound and Unbound Orbits

  • BOUND ORBIT – object does not have enough kinetic energy to escape

  • UNBOUND ORBIT – object can eventually reach d = ∞


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Escape Velocity

… minimum speed needed to escape to infinite distance


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