Download Solar System

Our Solar System
Chap. 29
Overview 29.1
Terrestrial Planets 29.2
Gas Giant Planets 29.3
Formation of Solar System 29.4
Overview – 29.1
Objectives
• describe early
models of our solar
system
• examine the
modern heliocentric
model of our solar
system
• relate gravity to
the motions of
celestial bodies
http://www.thesolutionsite.com/
I. What’s a Planet?
Dactyl – orbiting Ida
http://www.jpl.nasa.gov/
This has recently been debated.
I. What’s a Planet?
A. Current Criteria
I. What’s a Planet?
A. Current Criteria
1.
Orbits a star
2.
Above a certain size
3.
Not big enough to do fusion
I. What’s a Planet?
A. Current Criteria
B. How do you recognize a planet in
space?
http://www.astropics.com/
I. What’s a Planet?
A. Current Criteria
B. How do you recognize a planet in
space?
1.
See star chart
I. What’s a Planet?
A. Current Criteria
B. How do you recognize a planet in
space?
1.
See star chart
2.
Planets change position relative to
stars
II. Planetary Motion
II. Planetary Motion
A. Generally to the East
II. Planetary Motion
A. Generally to the East
B. Retrograde motion observed
II. Planetary Motion
A. Generally to the East
B. Retrograde motion observed
1. To explain this Copernicus/astronomers
embraced heliocentric model.
II. Planetary Motion
A. Generally to the East
B. Retrograde motion observed
1. To explain this Copernicus/astronomers
embraced heliocentric model.
2. Inner planets go faster and pass out
planets.
III. Kepler’s Laws
http://www-gap.dcs.st-and.ac.uk/~history
III. Kepler’s Laws
A. First Law – planets orbit the sun
in an ellipse (oval shape)
III. Kepler’s Laws
A. First Law – planets orbit the sun
in an ellipse (oval shape)
1. Ellipse has two ‘centers’ called
.
III. Kepler’s Laws
A. First Law – planets orbit the sun
in an ellipse (oval shape)
1. Ellipse has two ‘centers’ called foci.
2. In our solar system,
always at one of the foci.
is
III. Kepler’s Laws
A. First Law – planets orbit the sun
in an ellipse (oval shape)
1. Ellipse has two ‘centers’ called foci.
2. In our solar system, our sun is
always at one of the foci.
3. Line the goes through both foci and
the ellipse is called the
.
III. Kepler’s Laws
A. First Law – planets orbit the sun
in an ellipse (oval shape)
1. Ellipse has two ‘centers’ called foci.
2. In our solar system, our sun is
always at one of the foci.
3. Line the goes through both foci and
the ellipse is called the major axis.
4. The average distance of an orbiting
body is equal to the
.
III. Kepler’s Laws
A. First Law – planets orbit the sun
in an ellipse (oval shape)
1. Ellipse has two ‘centers’ called foci.
2. In our solar system, our sun is
always at one of the foci.
3. Line the goes through both foci and
the ellipse is called the major axis.
4. The average distance of an orbiting
body is equal to the semi-major axis.
5. For Earth-Sun this is 1.496 x 108 km
= 1 AU (
)
III. Kepler’s Laws
A. First Law – planets orbit the sun
in an ellipse (oval shape)
1. Ellipse has two ‘centers’ called foci.
2. In our solar system, our sun is
always at one of the foci.
3. Line the goes through both foci and
the ellipse is called the major axis.
4. The average distance of an orbiting
body is equal to the semi-major axis.
5. For Earth-Sun this is 1.496 x 108 km
= 1 AU (astronomical unit)
III. Kepler’s Laws
A. First Law – planets orbit the sun
in an ellipse (oval shape)
6. Eccentricity = level of ‘ovalness’
Eccentricity =
Distance between foci
Length of major axis
III. Kepler’s Laws
A. First Law – planets orbit the sun
in an ellipse (oval shape)
6. Eccentricity = level of ‘ovalness’
a. If value is 0 the shape is
.
Eccentricity =
Distance between foci
Length of major axis
III. Kepler’s Laws
A. First Law – planets orbit the sun
in an ellipse (oval shape)
6. Eccentricity = level of ‘ovalness’
a. If value is 0 the shape is circle.
b. If value is 1 the shape is
Eccentricity =
Distance between foci
Length of major axis
.
III. Kepler’s Laws
A. First Law – planets orbit the sun
in an ellipse (oval shape)
6. Eccentricity = level of ‘ovalness’
a. If value is 0 the shape is circle.
b. If value is 1 the shape is parabola.
Eccentricity =
Distance between foci
Length of major axis
III. Kepler’s Laws
A. First Law – planets orbit the sun
in an ellipse (oval shape)
6. Eccentricity = level of ‘ovalness’
7. Perihelion/Aphelion
Perihelion is point
Aphelion is point
to the Sun.
from the Sun
III. Kepler’s Laws
A. First Law – planets orbit the sun
in an ellipse (oval shape)
6. Eccentricity = level of ‘ovalness’
7. Perihelion/Aphelion
Perihelion is point closest to the Sun.
Aphelion is point farthest from the Sun
III. Kepler’s Laws
A. First Law – planets orbit the sun
in an ellipse (oval shape)
6. Eccentricity = level of ‘ovalness’
7. Perihelion/Aphelion
#1
#2
III. Kepler’s Laws
A. First Law – planets orbit the sun
in an ellipse (oval shape)
6. Eccentricity = level of ‘ovalness’
7. Perihelion/Aphelion
8. Orbital period
Time is takes to complete an orbit
III. Kepler’s Laws
A. First Law – planets orbit the sun
in an ellipse (oval shape)
B. Second Law – Law of Areas
III. Kepler’s Laws
A. First Law – planets orbit the sun
in an ellipse (oval shape)
B. Second Law – Law of Areas
A line drawn between a planet and the Sun sweeps
out an equal area in equal amounts of time.
III. Kepler’s Laws
A. First Law – planets orbit the sun
in an ellipse (oval shape)
B. Second Law – Law of Areas
C. Third Law – a math relationship
p2
a3
=
III. Kepler’s Laws
A. First Law – planets orbit the sun
in an ellipse (oval shape)
B. Second Law – Law of Areas
C. Third Law – a math relationship
p2
a3
(Period (time) in Years)2
=
=
3
(Length in AU)
1
IV. Gravity
IV. Gravity
A. Any two bodies attract each other
with force proportional to . . .
IV. Gravity
A. Any two bodies attract each other
with force proportional to . . .
1. Mass (size) of each body
The bigger the masses the
force
the gravitational
IV. Gravity
A. Any two bodies attract each other
with force proportional to . . .
1. Mass (size) of each body
The bigger the masses the bigger the gravitational
force
IV. Gravity
A. Any two bodies attract each other
with force proportional to . . .
1. Mass (size) of each body
2. Distance between two bodies
The
the distance between the bodies, the
larger the gravitational force.
IV. Gravity
A. Any two bodies attract each other
with force proportional to . . .
1. Mass (size) of each body
2. Distance between two bodies
The smaller the distance between the bodies, the
larger the gravitational force.
IV. Gravity
A. Any two bodies attract each other
with force proportional to . . .
B. Equation
Fg
Gm1m2
=
d2
G = 6.67 X 10-11 m3/kg s2
IV. Gravity
A. Any two bodies attract each other
with force proportional to . . .
B. Equation
1. If the mass of one body is doubled then
the gravitational force is
.
Fg
Gm1m2
=
d2
G = 6.67 X 10-11 m3/kg s2
IV. Gravity
A. Any two bodies attract each other
with force proportional to . . .
B. Equation
1. If the mass of one body is doubled then
the gravitational force is doubled.
2. If the distance is doubled, then gravity
__________
Fg
Gm1m2
=
d2
G = 6.67 X 10-11 m3/kg s2
IV. Gravity
A. Any two bodies attract each other
with force proportional to . . .
B. Equation
1. If the mass of one body is doubled then
the gravitational force is doubled.
2. If the distance is doubled, then gravity
becomes ¼ .
Fg
Gm1m2
=
d2
G = 6.67 X 10-11 m3/kg s2
IV. Gravity
A. Any two bodies attract each other
with force proportional to . . .
B. Equation
C. Center of Mass
IV. Gravity
A. Any two bodies attract each other
with force proportional to . . .
B. Equation
C. Center of Mass
1. Planets orbit around the planet-Sun
center of mass.
IV. Gravity
A. Any two bodies attract each other
with force proportional to . . .
B. Equation
C. Center of Mass
1. Planets orbit around the planet-Sun
center of mass.
2. Center of mass is usually very close to
center of
.
IV. Gravity
A. Any two bodies attract each other
with force proportional to . . .
B. Equation
C. Center of Mass
1. Planets orbit around the planet-Sun
center of mass.
2. Center of mass is usually very close to
center of Sun.
The End
The Terrestrial Planets – 29.2
Objectives
• describe the
properties of the
terrestrial planets
• compare Earth with
the other terrestrial
planets
The Terrestrial Planets
• These planets are named terrestrial because
of their solid, rocky surfaces.
The Terrestrial Planets
• These planets are named terrestrial because
of their solid, rocky surfaces.
• These planets are sometimes called the
inner planets.
I. Mercury
I. Mercury
A. 1/3 the size of Earth.
I. Mercury
A. 1/3 the size of Earth.
B. Mercury rotates 1.5 x for every
orbit.
I. Mercury
A. 1/3 the size of Earth.
B. Mercury rotates 1.5 x for every
orbit.
C. It takes 88 days to complete orbit
(and days to rotate).
I. Mercury
A. 1/3 the size of Earth.
B. Mercury rotates 1.5 x for every
orbit.
C. It takes 88 days to complete orbit
(and 59 days to rotate).
D. Atmosphere is thin, made from
oxygen and sodium.
I. Mercury
A. 1/3 the size of Earth.
B. Mercury rotates 1.5 x for every
orbit.
C. It takes 88 days to complete orbit
(and 59 days to rotate).
D. Atmosphere is thin, made from
oxygen and sodium.
E. Large temperature fluctuations
(from 100 K to 700 K).
I. Mercury
F. Observed by Mariner in 1974 &
1975.
http://www.nasa.gov
I. Mercury
F. Observed by Mariner in 1974 &
1975.
G. Surface marked by craters and
by smooth plains.
http://www.nasa.gov
I. Mercury
F. Observed by Mariner in 1974 &
1975.
G. Surface marked by craters and
by smooth plains.
H. Dense (nickel – iron core). No
seismic data.
I. Mercury
F. Observed by Mariner in 1974 &
1975.
G. Surface marked by craters and
by smooth plains.
H. Dense (nickel – iron core). No
seismic data.
I. Weak magnetic field (1% of
Earth’s).
I. Mercury
F. Observed by Mariner in 1974 &
1975.
G. Surface marked by craters and
by smooth plains.
H. Dense (nickel – iron core). No
seismic data.
I. Weak magnetic field (1% of
Earth’s).
J. No moons
I. Mercury
K. Proximity to Sun makes it hard
to observe.
II. Venus
http://www.nasa.gov
II. Venus
A. Albedo is 0.75 (highest). Planet is
called evening star/morning star.
II. Venus
A. Albedo is 0.75 (highest). Planet is
called evening star/morning star.
B. Venus rotates slowly (= long days
– about 243 Earth days)
II. Venus
A. Albedo is 0.75 (highest). Planet is
called evening star/morning star.
B. Venus rotates slowly (= long days
– about 243 Earth days)
C. Spins clockwise (retrograde)
II. Venus
A. Albedo is 0.75 (highest). Planet is
called evening star/morning star.
B. Venus rotates slowly (= long days
– about 243 Earth days)
C. Spins clockwise (retrograde)
D. Thick clouds
II. Venus
A. Albedo is 0.75 (highest). Planet is
called evening star/morning star.
B. Venus rotates slowly (= long days
– about 243 Earth days)
C. Spins clockwise (retrograde)
D. Thick clouds
E. High Temperatures (737 K) and
high pressures (92 atm).
II. Venus
A. Albedo is 0.75 (highest). Planet is
called evening star/morning star.
B. Venus rotates slowly (= long days
– about 243 Earth days)
C. Spins clockwise (retrograde)
D. Thick clouds
E. High Temperatures (737 K) and
high pressures (92 atm).
F. Atmosphere is CO2 & N2.
II. Venus
G. Clouds made of H2SO4.
II. Venus
G. Clouds made of H2SO4.
H. Pioneer Venus and Magellan flew
by.
Magellan
http://www.nasa.gov
II. Venus
G. Clouds made of H2SO4.
H. Pioneer Venus and Magellan flew
by.
I. Smooth surface – few impact
craters
http://www.nasa.gov
http://www.nasa.gov
Venera 13 survived on the surface for 2
hours, 7 minutes, long enough to obtain 14
images on 1 March, 1982.
II. Venus
G. Clouds made of H2SO4.
H. Pioneer Venus and Magellan flew
by.
I. Smooth surface – few impact
craters
J. No water
II. Venus
G. Clouds made of H2SO4.
H. Pioneer Venus and Magellan flew
by.
I. Smooth surface – few impact
craters
J. No water
K. Similar makeup
and size to Earth
http://www.nasa.gov
II. Venus
G. Clouds made of H2SO4.
H. Pioneer Venus and Magellan flew
by.
I. Smooth surface – few impact
craters
J. No water
K. Similar makeup
and size to Earth
L. No moons
http://www.nasa.gov
III. Earth
III. Earth
A. Only planet with water in all 3
states.
http://www.nasa.gov
III. Earth
A. Only planet with water in all 3
states.
B. Moderate, dense atmosphere
creates ideal greenhouse effect.
III. Earth
A. Only planet with water in all 3
states.
B. Moderate, dense atmosphere
creates ideal greenhouse effect.
C. Precession – the Earth wobbles
every 26,000 y due to moon’s pull.
Precession
III. Earth
A. Only planet with water in all 3
states.
B. Moderate, dense atmosphere
creates ideal greenhouse effect.
C. Precession – the Earth wobbles
every 26,000 y due to moon’s pull.
D. Made of floating plates according
to
.
III. Earth
A. Only planet with water in all 3
states.
B. Moderate, dense atmosphere
creates ideal greenhouse effect.
C. Precession – the Earth wobbles
every 26,000 y due to moon’s pull.
D. Made of floating plates according
to tectonic theory.
IV. Mars (the red planet)
http://www.nasa.gov
IV. Mars (the red planet)
A. Smaller than Earth
http://www.nasa.gov
IV. Mars (the red planet)
A. Smaller than Earth
B. Contains the solar
system’s largest volcano
– Olympus Mons.
This is a shield volcano
that is the size of
Arizona. It is 5 x the
size of Mauna Kea, and
2.5 x the height.
http://www.nasa.gov
IV. Mars (the red planet)
A. Smaller than Earth
B. Contains the solar systems largest
volcano – Olympus Mons.
C. Large Canyon called Valles
Marineris.
http://www.nasa.gov
IV. Mars (the red planet)
A. Smaller than Earth
B. Contains the solar systems largest
volcano – Olympus Mons.
C. Large Canyon called Valles
Marineris.
D. Dry River Beds/Channels hint of
H2O.
Martian River Delta
http://www.nasa.gov
IV. Mars (the red planet)
A. Smaller than Earth
B. Contains the solar systems largest
volcano – Olympus Mons.
C. Large Canyon called Valles
Marineris.
D. Dry River Beds/Channels hint of
H2O.
E. Water Ice caps are under CO2 ice
caps at poles.
Martian North Pole - Summer
Martian South Pole
http://www.nasa.gov
IV. Mars (the red planet)
F. Atmosphere mostly CO2, but
pressure is low.
IV. Mars (the red planet)
F. Atmosphere mostly CO2, but
pressure is low.
G. Turbulent atmosphere conditions
create wind storms.
http://www.nasa.gov
IV. Mars (the red planet)
F. Atmosphere mostly CO2, but
pressure is low.
G. Turbulent atmosphere conditions
create wind storms.
H. Southern hemisphere is cratered,
highlands.
IV. Mars (the red planet)
F. Atmosphere mostly CO2, but
pressure is low.
G. Turbulent atmosphere conditions
create wind storms.
H. Southern hemisphere is cratered,
highlands.
I. Northern hemisphere is mostly
plains, few craters.
IV. Mars (the red planet)
F. Atmosphere mostly CO2, but
pressure is low.
G. Turbulent atmosphere conditions
create wind storms.
H. Southern hemisphere is cratered,
highlands.
I. Northern hemisphere is mostly
plains, few craters.
J. Core hypothesized to be solid Fe &
Ni.
IV. Mars (the red planet)
K. Mars has a 25º tilt creating seasons.
IV. Mars (the red planet)
K. Mars has a 25º tilt creating seasons.
L. Visited by Mariners 4 & 9, Viking
landers, and Exploration Rovers.
http://www.nasa.gov
Terrestrial Planets
• These closest planets to us are also most
similar to Earth.
http://www.nasa.gov
The End
The Gas Giant Planets – 29.3
Objectives
• Describe the
properties of the gas
giant planets
• Identify the unique
nature of the planet
Pluto
The Gas Giant Planets
• They are 15 to 300 x Earth’s size.
• Made primarily of lighter elements (hydrogen,
helium, carbon, nitrogen & oxygen).
• Inner are composed of fluid (liquids or gases)
http://www.nasa.gov
I. Jupiter
As Voyager 1 approached
Jupiter in 1979, it took images
of the planet at regular
intervals. This sequence is
made from 66 images taken
once every Jupiter rotation
period (about 10 hours). This
time-lapse movie uses images
taken every time Jupiter
longitude 68W passed under
the spacecraft.
http://www.nasa.gov
I. Jupiter
A. Largest planet in S.S. (70% of all
planetary mass is Jupiter).
I. Jupiter
A. Largest planet in S.S. (70% of all
planetary mass is Jupiter).
B. Jupiter has banded appearance.
http://www.nasa.gov
I. Jupiter
A. Largest planet in S.S. (70% of all
planetary mass is Jupiter).
B. Jupiter has banded appearance.
C. Visited by Pioneer 10 & 11,
Voyager 1 & 2, and Galileo.
http://www.nasa.gov
I. Jupiter
A. Largest planet in S.S. (70% of all
planetary mass is Jupiter).
B. Jupiter has banded appearance.
C. Visited by Pioneer 10 & 11,
Voyager 1 & 2, and Galileo.
D. Made of hydrogen and helium gas.
Closer to the center these gases
condense to liquid.
http://www.nasa.gov
I. Jupiter
A. Largest planet in S.S. (70% of all
planetary mass is Jupiter).
B. Jupiter has banded appearance.
C. Visited by Pioneer 10 & 11,
Voyager 1 & 2, and Galileo.
D. Made of hydrogen and helium gas.
Closer to the center these gases
condense to liquid.
E. Contains liquid metallic hydrogen
which generates magnetic field
I. Jupiter
F. Rotates fast (orbital period = 10 h,
shortest in S.S.)
I. Jupiter
F. Rotates fast (orbital period = 10 h,
shortest in S.S.)
G. Atmosphere
I. Jupiter
F. Rotates fast (orbital period = 10 h,
shortest in S.S.)
G. Atmosphere
1. Contains belts (low, warm, dark clouds)
& zones (high, cooler, light clouds)
I. Jupiter
F. Rotates fast (orbital period = 10 h,
shortest in S.S.)
G. Atmosphere
1. Contains belts (low, warm, dark clouds)
& zones (high, coller, light clouds)
2. Great red spot (GRS) is a giant, 300
year old storm.
The Great Red Spot is an anti-cyclonic (highpressure) storm on Jupiter that can be likened to the
worst hurricanes on Earth. An ancient storm, it is so
large that three Earths could fit inside it.
http://www.nasa.gov
I. Jupiter
F. Rotates fast (orbital period = 10 h,
shortest in S.S.)
G. Atmosphere
H. Moons
This has the most moons of any planet in our S.S.
I. Jupiter
F. Rotates fast (orbital period = 10 h,
shortest in S.S.)
G. Atmosphere
H. Moons
1. Galilean (4 largest: Io, Europa,
Ganymede, Callisto)
http://www.nasa.gov
I. Jupiter
F. Rotates fast (orbital period = 10 h,
shortest in S.S.)
G. Atmosphere
H. Moons
1. Galilean (4 largest: Io, Europa,
Ganymede, Callisto)
2. Lesser moons – there are about 60
This is the most moons of any planet in our S.S.
I. Jupiter
F. Rotates fast (orbital period = 10 h,
shortest in S.S.)
G. Atmosphere
H. Moons
I. Rings – Jupiter has a ring
discovered by Voyager. Distance =
6400 m across).
II. Saturn
http://www.nasa.gov
II. Saturn
A. Second largest planet
II. Saturn
A. Second largest planet
B. Visited by Pioneer 10 & 11,
Voyager 1 & 2, and Cassini.
http://www.nasa.gov
II. Saturn
A. Second largest planet
B. Visited by Pioneer 10 & 11,
Voyager 1 & 2, and Cassini.
C. Like Jupiter, has fast rotation (11
hours)
II. Saturn
A. Second largest planet
B. Visited by Pioneer 10 & 11,
Voyager 1 & 2, and Cassini.
C. Like Jupiter, has fast rotation (11
hours)
D. Atmosphere primarily hydrogen,
helium and ammonia ice
II. Saturn
A. Second largest planet
B. Visited by Pioneer 10 & 11,
Voyager 1 & 2, and Cassini.
C. Like Jupiter, has fast rotation (11
hours)
D. Atmosphere primarily hydrogen,
helium and ammonia ice
E. Contains belts and zones
II. Saturn
F. Characterized by rings
http://www.nasa.gov
II. Saturn
F. Characterized by rings
1. Rings are rock and ice (dust sized to car
sized).
II. Saturn
F. Characterized by rings
1. Rings are rock and ice (dust sized to car
sized).
2. There are 7 major rings
II. Saturn
F. Characterized by rings
1. Rings are rock and ice (dust sized to car
sized).
2. There are 7 major rings
3. Rings don’t coalesce into single mass
(moon) because they are too close.
II. Saturn
F. Characterized by rings
1. Rings are rock and ice (dust sized to car
sized).
2. There are 7 major rings
3. Rings don’t coalesce into single mass
(moon) because they are too close.
4. Origin probably from destruction of a
moon.
II. Saturn
F. Characterized by rings
G. Moons
II. Saturn
F. Characterized by rings
G. Moons
1. Titan – largest (bigger than our moon)
http://www.nasa.gov
II. Saturn
F. Characterized by rings
G. Moons
1. Titan – largest (bigger than our moon)
2. There are 7 intermediate and about 40
more moons.
III. Uranus
http://www.nasa.gov
III. Uranus
A. 7th planet – discovered in 1781
III. Uranus
A. 7th planet – discovered in 1781
B. Contains methane in atmosphere,
giving it a bluish appearance
III. Uranus
A. 7th planet – discovered in 1781
B. Contains methane in atmosphere,
giving it a bluish appearance
C. Atmosphere also contains hydrogen
and helium
III. Uranus
A. 7th planet – discovered in 1781
B. Contains methane in atmosphere,
giving it a bluish appearance
C. Atmosphere also contains hydrogen
and helium
D. No belts & zones/no distinct clouds
III. Uranus
A. 7th planet – discovered in 1781
B. Contains methane in atmosphere,
giving it a bluish appearance
C. Atmosphere also contains hydrogen
and helium
D. No belts & zones/no distinct clouds
E. The poles lie in the orbital plane
(planet was knocked sideways)
http://www.nasa.gov
An infrared composite image of the two hemispheres of Uranus obtained with Keck
adaptive optics. The images were obtained on July 11 and 12, 2004. The North pole
is at 4 o'clock.
III. Uranus
A. 7th planet – discovered in 1781
B. Contains methane in atmosphere,
giving it a bluish appearance
C. Atmosphere also contains hydrogen
and helium
D. No belts & zones/no distinct clouds
E. The poles lie in the orbital plane
(planet was knocked sideways)
F. Contains 27 moons named after
Shakespearean characters
III. Uranus
G. Moons orbit in equatorial plane
http://www.nasa.gov
III. Uranus
G. Moons orbit in equatorial plane
H. Rings are very dark, hard to discover
http://www.nasa.gov
III. Uranus
G. Moons orbit in equatorial plane
H. Rings are very dark, hard to discover
I.
Visited by Voyager 2
III. Uranus
G. Moons orbit in equatorial plane
H. Rings are very dark, hard to discover
I.
Visited by Voyager 2
J.
Orbit takes about 84 years
IV. Neptune
IV. Neptune
A. Predicted before it was discovered
based on gravity pull on Uranus
IV. Neptune
A. Predicted before it was discovered
based on gravity pull on Uranus
B. Visited by Voyager 2
IV. Neptune
A. Predicted before it was discovered
based on gravity pull on Uranus
B. Visited by Voyager 2
C. Like Uranus, contains methane giving
a bluish color
IV. Neptune
A. Predicted before it was discovered
based on gravity pull on Uranus
B. Visited by Voyager 2
C. Like Uranus, contains methane giving
a bluish color
D. Contains clouds, belts and zones
IV. Neptune
A. Predicted before it was discovered
based on gravity pull on Uranus
B. Visited by Voyager 2
C. Like Uranus, contains methane giving
a bluish color
D. Contains clouds, belts and zones
E. A great dark spot appeared on
Neptune, but disappeared in 1994
http://www.nasa.gov
IV. Neptune
F. Has about 13 moons including Triton
http://www.nasa.gov
IV. Neptune
F. Has about 13 moons including Triton
1. Triton undergoes retrograde orbit
(moon orbits opposite to Neptune’s
rotation)
IV. Neptune
F. Has about 13 moons including Triton
1. Triton undergoes retrograde orbit
(moon orbits opposite to Neptune’s
rotation)
2. Triton has nitrogen geysers
V. Pluto
http://www.nasa.gov
V. Pluto
A. Solid surface (though not classified
terrestrial because of low density)
V. Pluto
A. Solid surface (though not classified
terrestrial because of low density)
B. Too small to be a gas giant
V. Pluto
A. Solid surface (though not classified
terrestrial because of low density)
B. Too small to be a gas giant
C. Very eccentric orbit
V. Pluto
A. Solid surface (though not classified
terrestrial because of low density)
B. Too small to be a gas giant
C. Very eccentric orbit
D. Tipped over so that North pole faces
South
V. Pluto
A. Solid surface (though not classified
terrestrial because of low density)
B. Too small to be a gas giant
C. Very eccentric orbit
D. Tipped over so that North pole faces
South
E. Has a moon (Charon) that is about
the same size
V. Pluto
F. New Horizons recently launched
destined for Pluto in 2015.
The End
Formation of Our Solar
System – 29.4
Objectives
• Summarize the
properties of the solar
system that support the
theory of SS formation
• Describe how the planets
formed from a disk
surrounding your Sun
• Explore remnants of
solar system
Review of Solar System
I. Observations that need
explanations
I. Observations that need
explanations
A. Most planets have nearly circular
orbits in same direction
I. Observations that need
explanations
A. Most planets have nearly circular
orbits in same direction
B. Some planets are terrestrial close
to sun while jovian planets are
further
I. Observations that need
explanations
A. Most planets have nearly circular
orbits in same direction
B. Some planets are terrestrial close
to sun while jovian planets are
further
C. Some planets have moons while
other do not
II. Origins
II. Origins
A. Interstellar clouds
http://ase.tufts.edu/astroweb
II. Origins
A. Interstellar clouds
1. Exist in space between stars
II. Origins
A. Interstellar clouds
1. Exist in space between stars
2. Made of H & He and dust
II. Origins
A. Interstellar clouds
1. Exist in space between stars
2. Made of H & He and dust
3. Very low pressure
II. Origins
A. Interstellar clouds
B. The collapse of interstellar cloud
II. Origins
A. Interstellar clouds
B. The collapse of interstellar cloud
1. Gases condense
II. Origins
A. Interstellar clouds
B. The collapse of interstellar cloud
1. Gases condense
2. Spin is magnified
II. Origins
A. Interstellar clouds
B. The collapse of interstellar cloud
1. Gases condense
2. Spin is magnified
3. Cloud is flattened to disc shape
II. Origins
A. Interstellar clouds
B. The collapse of interstellar cloud
C. Solar Nebula – our dust which
formed around the sun
http://www.nasa.gov
II. Origins
A. Interstellar clouds
B. The collapse of interstellar cloud
C. Solar Nebula – our dust which
formed around the sun
1. Warmest temps were
the sun
II. Origins
A. Interstellar clouds
B. The collapse of interstellar cloud
C. Solar Nebula – our dust which
formed around the sun
1. Warmest temps were near the sun
2. Coolest temps were
the sun
II. Origins
A. Interstellar clouds
B. The collapse of interstellar cloud
C. Solar Nebula – our dust which
formed around the sun
1. Warmest temps were near the sun
2. Coolest temps were far from the sun
II. Origins
A. Interstellar clouds
B. The collapse of interstellar cloud
C. Solar Nebula – our dust which
formed around the sun
D. Object grow
II. Origins
A. Interstellar clouds
B. The collapse of interstellar cloud
C. Solar Nebula – our dust which
formed around the sun
D. Object grow
1. Gravity pulls material together
II. Origins
A. Interstellar clouds
B. The collapse of interstellar cloud
C. Solar Nebula – our dust which
formed around the sun
D. Object grow
1. Gravity pulls material together
2. Eventually planetesimals form
II. Origins
A. Interstellar clouds
B. The collapse of interstellar cloud
C. Solar Nebula – our dust which
formed around the sun
D. Object grow
1. Gravity pulls material together
2. Eventually planetesimals form
3. Collisions and mergers destroyed
planetesimals until few remain
II. Origins
E. Jupiter forms first
II. Origins
E. Jupiter forms first
1. Accumulates most of nearby material
II. Origins
E. Jupiter forms first
1. Accumulates most of nearby material
2. Some material remains in equatorial
disk (rings/moons)
II. Origins
E. Jupiter forms first
F. Terrestrial Planets
II. Origins
E. Jupiter forms first
F. Terrestrial Planets
1. Refractory material (Metals/rocks)
condense at higher temperatures
II. Origins
E. Jupiter forms first
F. Terrestrial Planets
1. Refractory material (Metals/rocks)
condense at higher temperatures
2. Gas near Sun becomes part of Sun
II. Origins
E. Jupiter forms first
F. Terrestrial Planets
1. Refractory material (Metals/rocks)
condense at higher temperatures
2. Gas near Sun becomes part of Sun
3. Solar wind blows away nearby gases
http://www.nasa.gov
III. Asteroids
A. Interplanetary rocks/debris that
orbit the Sun
http://www.nasa.gov
III. Asteroids
A. Interplanetary rocks/debris that
orbit the Sun
1. Thought to be left-over pieces of
planetesimals
III. Asteroids
A. Interplanetary rocks/debris that
orbit the Sun
1. Thought to be left-over pieces of
planetesimals
2. Jupiter’s gravity interferes with
process of coalescing
IV. Meteoroids
IV. Meteoroids
A. Asteroids may collide and their
debris may reach Earth
IV. Meteoroids
A. Asteroids may collide and their
debris may reach Earth
B. A
is a streak of light
formed by this debris in
atmosphere
IV. Meteoroids
A. Asteroids may collide and their
debris may reach Earth
B. A meteor is a streak of light
formed by this debris in
atmosphere
C. A
is the material that
occasionally reaches Earth’s
surface
IV. Meteoroids
A. Asteroids may collide and their
debris may reach Earth
B. A meteor is a streak of light
formed by this debris in
atmosphere
C. A meteorite is the material that
occasionally reaches Earth’s
surface
V. Comets
Comet C/2002 V1
V. Comets
A. Have highly eccentric orbits
V. Comets
A. Have highly eccentric orbits
B. Nucleus made of ice/rock
V. Comets
A. Have highly eccentric orbits
B. Nucleus made of ice/rock
C. Glowing gases around nucleus is
called the coma
V. Comets
A. Have highly eccentric orbits
B. Nucleus made of ice/rock
C. Glowing gases around nucleus is
called the coma
D. Tail always points away from Sun
due to solar rays hitting it.
The End