Download Ch. 27 Notes

STARS AND PLANETS
Lesson 1
WHAT IS A NEBULA
A nebula is the
birthplace of a star.
Consists of a large
cloud of hydrogen
and helium.
TYPES OF NEBULAS
Planetary Nebulas
They have nothing
to do with planets
they just look like
one in a small
telescope.
Form from a
supernova
explosion
EMISSION NEBULA
Emission nebulae
are clouds of high
temperature gas.
The atoms in the
cloud are energized
by ultraviolet light
from a nearby star
and emit radiation
as they fall back
into lower energy
states
Often colored Red
DARK NEBULA
Dark nebulae are
clouds of dust
which are simply
blocking the light
from whatever is
behind
REFLECTION
NEBULA
Reflection
nebulae are
clouds of dust
which are simply
reflecting the light
of a nearby star or
stars.
Often radiate blue
LIFE CYCLE OF A STAR
All stars
originate in a
nebula
Nebulas pull
hydrogen and
helium using
gravity and
these elements
condense to
form a star.
PROTOSTAR
A protostar is
a dense
collection of
gas.
As gravity
pulls in H and
He it will
begins to
flatten and
spin.
CHECK FOR UNDERSTANDING

What are nebulas?

What is the chemical composition of a nebula?

Why are nebulas significant to the universe?
Complete answers with complete sentences and IN
YOUR OWN WORDS!!!
STAGE 1
When a nebula reaches about
100,000,000 years old it begins
to form a protostar.
When the protostar reaches
18,000,000 degrees F nuclear
fusion of hydrogen begins to
form helium.
The larger the star, the shorter
the star will live.
OUR SUN
A star like our sun began in a
nebula.
Friction and gravity pull elements
together and a star is formed.
Our star (the sun) is within the main
sequence.
STAGE 2:
MAIN
SEQUENCE
A star spend 90% of its life within the main sequence
During this stage nuclear fusion continues forming helium from the
fusion of hydrogen.
STAGE 3
When the star has spent
nearly all of the hydrogen
into helium the star enters
the third stage.
LEAVING STAGE
3
Depending upon the size of the
star there are two options.
1.
Turns into a Red Giant and
then back to a nebula
Or
2. Turns into a Red
Supergiant and then
explodes into a supernova.

Red Giant

The core of the star
contracts because it is
converting gravitational
energy into thermal
energy.

This flood of energy
pushes toward the
surface and the outer
shell of the star expands
– the star now is referred
to as a red giant.
LEAVING THE MAIN
SEQUENCE – 3RD STAGE
RED GIANT
COMPARISON
STARS
BALANCING ACT
The outward pressures of
the radiation from nuclear
fusion resist the inward
pull of gravity.
When equilibrium is met,
the star becomes stabile
in size.
STARS BALANCING
ACT
A star’s size is determined by
its ability to balance heat and
gravity.
Gravity increases as the size
of the star increases.
The size of the star increases
based on how much
hydrogen it is fusing at its
core.
SUPERNOVA
When the star reaches the fusion of Iron the stars
gravitational force exceeds the outward force and the
star collapses upon itself and explodes.
CLOSEST STAR TO
EARTH
- ALPHA
CENTAURI
(4.24 LIGHTYEARS AWAY)
ETA CARINAE IS A
RARE “HYPER”GIANT A ONE OF A
KIND STAR THAT IS
SIMPLY TOO BIG.
IT’S MASS - ABOUT
100 TIMES GREATER
THAN OUR SUN AND AN EXCELLENT
CANDIDATE FOR A
SUPERNOVA.
BETELGEUSE IS ABOUT
100,000 TIMES
BRIGHTER THAN THE
SUN AND 1,000 TIMES
LARGER.
BETELGEUSE WOULD
EXTEND OUT TO THE
ORBIT OF JUPITER
ABOUT 1 MILLION
YEARS LEFT OF
NUCLEAR FUEL.
Herschel Space
Observatory 2013
CHECK FOR UNDERSTANDING
 Describe
the birth of a star?
 How
are stars and planets different? How are
they similar?
 Why
are stars significant to the universe?
Complete answers with complete sentences
and IN YOUR OWN WORDS!!!
R Sculptoris (Red Giant) – using ALMA – Atacama radio telescope)
 Quickly
heat
continues to build
up as the star tries
to fuse carbon and
oxygen.
 This
results in cosmic
burps – allowing the
atmosphere to
quietly eject its shell
outward into a
planetary nebula.
LESSON 2 - FINAL STAGES
OF A STAR (STAGE 4)
 The
core then begins to
contract due to gravity
and is compressed into
the size of our Earth.
 Creating
a very dense
and now a retired star.
Lucy 2,500 mi
diameter
BPM37093
FINAL STAGES OF A
STAR – STAGE 4
PLANETARY NEBULA – WHITE DWARFS
Helix Nebula is a planetary
nebula approximately 700
light-years away
PLANETARY NEBULA – WHITE DWARFS
Nebula Abell 39 - 7,000 lightyears distant toward the
constellation Hercules
PLANETARY NEBULA – WHITE DWARFS
Planetary Nebula IC 1295
 If
the star is
substantial in size
(4x the mass of our
sun) at the point of
impasse, its gases
will actually
implode.
 Similar
to a building
being demolished.
FINAL STAGES OF A
STAR – STAGE 4
PLANETARY NEBULA - SUPERNOVA
SN 1572 - Tycho's
 Resulting
SN 1054
in a supernova and leaving behind a very
dense Neutron star and a planetary nebula full of
heavier elements like gold and silver.
PLANETARY NEBULA – SUPERNOVA
SN 1987a
OUR SUN
 The
sun is made up of a matter called plasma.
 Most


abundant elements in the sun are (Horizons, 2012)
Hydrogen – 91%
Helium – 8.9%
OUR SUN
 Our
 It
star - is by far the largest object in the solar system
contains more than 99.8% of the total mass of the
Solar System (Jupiter contains most of the rest).
 The
Sun does rotate,
once every 25 days.
 Slower
at the poles;
as much as 36 days.
 This
odd behavior is
due to the fact that
the Sun is not a solid
body like the Earth.
OUR SUN
CHECK FOR UNDERSTANDING
 Why
is our Sun important to our solar system?
 What
is the composition of the Sun?
Complete answers with complete sentences
and IN YOUR OWN WORDS!!!
HERTZSPRUNG
- RUSSELL
DIAGRAM
 The
Hertzsprung-Russell Diagram is a graphical tool
that astronomers use to classify stars according to
their luminosity, spectral type, color, temperature and
evolutionary stage.
 Most
stars follow a sequence in their life in which the
go from hot to cool and luminous to dull.
SUN ANALOGY
 The
Sun’s primary fuel
source is hydrogen
fusion.
 Referred
to as nuclear
fusion- it is the process by
which nuclei combine to
form a new, more
massive nucleus creating
energy in the process.
 All
elements greater then
Lithium (#3) have been
formed by nuclear fusion
in stars.*
SUN AND NUCLEAR
FUSION
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 At
the center of the sun
the core makes up 25%
of the sun’s total
diameter of 864, 000
miles.
 The
temperature of the
core is about 28 million
ºF.
 The
surface is about
10,000 ºF
THE CORE OF THE SUN
 The
sun is a
typical middle
size star on the
Hertzsprung
diagram (G2V).
 The
sun is in its
prime it has spent
5 billion years on
the main
sequence of
stellar life, it has 5
billion years to go
before its rapidly
decays.
OUR SUN (STAR) ON A
HERTZSPRUNG DIAGRAM

Astronomers learn about
stars by analyzing the light
that the stars emit.

Starlight passing through a
spectrograph produces a
display of colors and lines
called a spectrum.
ANALYZING STARLIGHT
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TEMPERATURE
RANGE OF STARS
 Stars
are categorized like our light spectrum - Blue being
hottest, Red stars are coolest.
A
Blue star would have and average surface temp. of
63,000˚F, while a red star would have and average
surface temp. of 5,400˚F
 Our
Sun is a yellow star with average surface temp. of
10,000°F
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CHECK FOR UNDERSTANDING

What is the Hertzsprung Russell Diagram?

Draw the difference between Nuclear Fusion
and Nuclear Fission?
Complete answers with complete sentences and
IN YOUR OWN WORDS!!!
A
galaxy is a
collection of stars,
dust, and gas bound
together by gravity.*
 Galaxies
are made
of billions of stars
and comprise most
of the visible mass of
the universe.*
LESSON 3 –
GALAXIES
SPECTROSCOPY –WONDERS OF THE UNIVERSE
DOPPLER EFFECT
DOPPLER ON SHOW
UNIVERSE’S
AGE
 Detailed
observations estimate the universe formed
about 13.8 (Planck Collaboration, 2013) billion years ago.
OLDEST
SEEN
GALAXY

Galaxy named UDFy -38135539, spotted by the Hubble
2009 is oldest to date 13.1 billion years old (BYO).

Hubble has found others, but scientists need better
technology (Webb ’14) will feature infrared technology.
HOW DO
WE SEE
OLD
GALAXIES
 Very
difficult – if lucky gravitational lensing can be used
when a galaxy's image is being magnified by the gravity
of a massive cluster of galaxies parked in front of it,
making it appear 11 times brighter.

A light year is a measure
of distance, not time.

It is the distance that light,
which travels in a vacuum
at the rate of 186,000
miles per second, can
travel in a year.

This is equal to 5,870 trillion
miles.
WHAT IS A LIGHT
YEAR?
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CHECK FOR UNDERSTANDING

What is a light year?

What is Gravitational Lensing?
Complete answers with complete sentences and
IN YOUR OWN WORDS!!!

Galaxies are classified by
shape into three main
types.

1. A spiral galaxy (like our
own) has a nucleus of
bright stars and flattened
arms that spiral around the
nucleus.

About 77% of the
observed galaxies in the
universe are spiral
galaxies.
Grand Spiral Galaxy NGC 1232
THREE TYPES OF
GALAXIES
1. SPIRAL (& BARRED)
GALAXIES
Elliptical Galaxy M87
 Have
a large range of
sizes from over a million
light-years in diameter
to less than one-tenth
the size of our own Milky
Way.
 Very
little gas and dust
within and typically
associated with being
an older galaxy since
most of their stars are
old.
2. ELLIPTICAL
GALAXIES
 They
have no
particular shape,
and are fairly rich
in dust and gas.
3. IRREGULAR
GALAXIES
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3. IRREGULAR
GALAXIES
 Irregular
galaxies are usually found in groups or clusters,
where collisions and near-misses between galaxies are
common.
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
Types of galaxies according to the Hubble classification
scheme. An E indicates a type of elliptical galaxy; an S is
a spiral; and SB is a barred-spiral galaxy.
HUBBLE GALAXIES
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 We
are Located in
the Milky Way, has
a diameter of
about 100,000
light-years and
may contain more
than 200 billion
stars.
OUR MILKY WAY
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 It
a spiral galaxy in
which the sun is one of
hundreds of billions of
stars and rotates
510,000 mph making
one complete circuit
every 230 million years.
OUR MILKY WAY
DOPPLER EFFECT
 The
spectrum of a galaxy that is moving toward or away
from Earth appears to shift, due to the Doppler effect.
 Doppler
effect is an observed change in the frequency of
a wave when the source or observer is moving.
 It
is commonly heard when a vehicle sounding a siren or
horn approaches, passes, and recedes from an observer.
CHECK FOR UNDERSTANDING
Provide an example of a Doppler Effect and be
prepared to explain your example to the class.
Name and describe the 3 types of Galaxies and
draw each type.
Complete answers with complete sentences and
IN YOUR OWN WORDS!!!
BLUE SHIFT
& RED
SHIFT OF A
STAR
GEORGIA EDU.
 Galaxies
moving toward Earth are shifted slightly toward
blue, which is called blue shift.
 Galaxies
moving away from Earth are shifted slightly
toward red, which is called red shift.
 Cosmologists
and astronomers
can use the light
given off by an
entire galaxy to
create the
spectrum for
that galaxy.
GALAXY
SPECTRUM

(1889-1953) American
astronomer confirmed the
existence of galaxies other
than the Milky Way.

Using the largest telescope
on Earth (Mt. Wilson) he
deduced that the farther
away the galaxy, the faster
it was moving away from
us.

This relation, known as
Hubble’s Law, was
observational proof that
the universe was
expanding.
EDWIN HUBBLE
THE EXPANDING
UNIVERSE
 Using
Hubble’s observations and the latest technologies,
astronomers have been able to confirm that the
universe is expanding.
THE BIG
BANG
The most accepted theory to date that explains why we are
expanding is known as the Big bang theory.

It explains that all matter and energy in the universe was
compressed into an extremely small volume that 13.8 billion
years ago exploded and began expanding in all directions.

CHECK FOR UNDERSTANDING

What are the Red Shifts and Blue Shifts and how
do scientist use these to explore and understand
our universe?

How do astronomers know the universe is
expanding.
Complete answers with complete sentences and
IN YOUR OWN WORDS!!!
LESSON 4
FORMATION
OF OUR
SOLAR SYSTEM
 Our
 It
solar system is 4.6 billion years old.
was created by fragments of an interstellar gas
clouds (solar nebula).
FORMATION
OF PLANETS
 This
cloud would have been mostly hydrogen with
some helium and small amounts of the heavier
elements – which is what you see in the composition of
the Sun.

The solar nebular
theory (SNT) supposes
that planets form in
the rotating disks of
gas and dust around
our young star.

Proof- the sun, planets
and moons mostly
revolve and rotate in
the same direction.

The planet orbits, for
the most part, lie
close to a common
plane.
SOLAR NEBULAR THEORY
SOLAR NEBULAR
THEORY
 When
the sun became hot enough, the remaining gas
and dust were blown away into space, leaving the
planets orbiting the sun.
CLEARING THE
NEBULA
 Occurs
because of the sun’s radiation pressure and
strong surging wind from the young sun.
 Planets
would help clear the nebula by sweeping up the
remaining space debris.
ORIGIN OF THE SOLAR SYSTEM
 The
major factor in the origin of the solar system is
temperature.
ORIGIN OF THE
SOLAR SYSTEM
 The
inner nebula was hot, and only metals and rock
could condense there.
 The
cold outer nebula could form from lots of ices along
with metals and rocks.
ORIGIN OF
THE SOLAR
SYSTEM
 The
ice “frost” line seems to have between Mars and
Jupiter, and it separates the region for formation of
the high-density Terrestrial planets from that of the
low-density Jovian planets.
DENSITY
DIFFERENCES
OF THE
PLANETS
 The
variation in densities is an important clue to
understanding the making of the solar system.
 The
four inner planets are small with high densities while
the four outer planets are large and have low densities.
INNER
PLANETS
 The
heavier density is due to larger percentages of heavy
elements, such as iron, magnesium and aluminum.
 The
inner Terrestrial planets are Mercury, Venus, Earth,
and Mars.
OUTER
PLANETS
 The
outer planets are rich in low density gases like
hydrogen and helium.
 They
four outer Jovian (Gas Giants) are Jupiter, Saturn,
Uranus, and Neptune.
ORIGIN
OF THE
SOLAR
SYSTEM
 Technically
 It
Saturn is so light…
can float on water.
PLUTO

Declassified in 2006 as a
planet to dwarf planet,
asteroid number 134340.

In order to be a planet
there are 3 rules.
 (1) Must orbit a Star
 (2) Have sufficient
mass so that it is round
in shape
 (3) has cleared the
neighborhood around
its orbit.
PLUTO
KUIPER
BELT

Use picture to show a clear neighborhood
 Kuiper
belt a region of the solar system that is just
beyond the orbit of Neptune and that contains small
bodies made mostly of ice.
 Including
dwarf planets of Eris and Pluto.
 Asteroids
are
understood to be the
last remains of the
rocky planetesimals
that formed in the
warmer inner solar
system and therefore
could not incorporate
much ice.
 Most
are between
Mars and Jupiter –
including Ceres
(another Dwarf
planet).
ASTEROIDS
COMETS
 Comets
are quite small and composed of a fluffy mixture
of ice, dust and significant amounts of empty space.
 They
easily break apart when they pass by the Sun and
are believed to have formed in the cold outer solar
system, the huge comet cloud known as the Oort Cloud.
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OORT CLOUD
 The
Oort Cloud is
considered the
edge of the Sun's
orb of physical and
gravitational
influence and
answers the
question where do
comets come
from?
OORT CLOUD
 When
Earth first
formed, it was very
hot but over time
cooled to form
three distinct layers.
 In
a process called
differentiation,
denser materials
sank to the center,
and less dense
materials were
forced to the outer
layers.
LESSON 5 –
EARLY SOLID EARTH
RESONANCE WINE GLASS
MYTH BUSTER BRIDGE
 The
center is a
dense core
composed mostly
of iron and nickel.
 Around
the core is
a very thick layer of
iron- and
magnesium-rich
rock called the
mantle.
 The
outermost layer
of Earth is a thin
crust of less dense,
silica-rich rock.
EARLY SOLID EARTH
 Eventually,
Earth’s
surface cooled enough
for solid rock to form
from less dense
elements that were
pushed toward the
surface during
differentiation.
PRESENT DAY EARTH
 The
Earth
formed 4.6
billion years ago
(BYA), at this
point, it was
nothing more
than a molten
ball of rock
surrounded by
an atmosphere
of hydrogen
and helium.
EARTH’S EARLY
ATMOSPHERE
EARTH’S
EARLY
ATMOSPHERE
 In
the beginning the Earth did not have a magnetic
field to protect it.
 The
intense solar wind along with the collision with the
moon blew this early 1st atmosphere away.
 2nd
atmosphere formed
through outgassing of
active volcanoes as
Earth cooled to form a
solid crust (4.4 BYA).
 These
volcanoes
spewed out gasses, like
water vapor, carbon
dioxide and ammonia.
OUTGASSING

Light from the Sun broke
down the ammonia
molecules released by
volcanoes, releasing
nitrogen into the
atmosphere.

Over billions of years,
the quantity of nitrogen
built up to the levels we
see today.
ORIGIN OF NITROGEN
 Although
life formed
just a few hundred
million years later, it
was not until the
evolution of bacteria
3.5 billion years ago
that really changed
the early Earth
atmosphere into the
one we know today.
ORIGIN OF OXYGEN
 Fossils
of early
bacteria at least 3.4
BYA (HORIZONS 2012)
known as
cyanobacteria
(stromatolites)–
would have used
energy from the Sun
for photosynthesis,
and release oxygen
as a byproduct.
 They
also
sequestered carbon
dioxide in organic
molecules.
ORIGIN OF OXYGEN
 Over
hundreds of
millions of years, this
bacteria would
completely change the
Earth’s atmosphere
composition, bringing
us to our current mixture
of 21% oxygen and 78%
nitrogen.
ORIGIN OF OXYGEN
 The
abundance
of oxygen (O2)
would also create
a special oxygen
molecule known
as ozone (O3) in
the stratosphere.
 Most
ecosystems
rely on the ozone
to protect them
from harmful
ultraviolet
(UV) light from the
Sun.
OZONE IN EARTH’S
PRESENT ATMOSPHERE

Scientists believe Earth’s
water was delivered
sometime after the planet
formed.

Close proximity to the sun
would have boiled off
water inside rocks that
were part of the original
building materials
(assuming that is where
we started).
FORMATION OF EARTH
OCEANS
FORMATIO
N OF EARTH
OCEANS
 So
far water (ice) found on most comets does not match
water on Earth. (deuterium (2H) = heavy hydrogen D2O)
 Some
think asteroids were the primary source of water
HOW EARTH
RECEIVED WATER –
THE LATE HEAVY
BOMBARDMENT
 One
theory that would
explain the existence of
foreign water is known as
the Nice Model.
HOW EARTH
RECEIVED
WATER – THE
LATE HEAVY
BOMBARDM
ENT
 The
Nice Model postulates that the planets formed in a
much more compact configuration and that the
planets started crossing one another due to the 2:1
synchronous resonance of Jupiter and Saturn 3.9 BYA.
 This
resonance would scatter Uranus and Neptune into
their current orbits around the Sun and also disrupted
the ice particles of the Kuiper Belt creating the “Late
Heavy Bombardment” or cosmic pinball machine.
HOW EARTH RECEIVED WATER
 Hal
Levison is
a planetary scientist
(Colorado) and worked
on the Nice Model.
 While
asteroids remain
a prime suspect
scientist have found
some proof from Kuiper
Belt Comet Hartley 2,
that comets can have
the same water
chemistry that matches
Earth (Klotz 2011).
HOW EARTH
RECEIVES WATER
 Most
scientists agree on the
Giant Impact Hypothesis
which states that the
formation of the moon
began when a large object
(Thea) collided with Earth
around 4.5 bya.
 This
hypothesis would explain
why moon rocks share many
of the same chemical
characteristics of Earth’s
mantle.
LESSON 6 - THE
CREATION OF OUR
MOON
 Rocks
from the lunar
terrae, “lands” are lightcolored, coarse-grained
and contain calcium and
aluminum.
 Rocks
from the maria,
“seas” are dark-colored
fine-grained basalts and
contain titanium,
magnesium, and iron.
THE LUNAR
ANATOMY
 Craters
abound on the
moon, at least 30,000 of
them boasting a
diameter greater then
0.6 miles.
 Most
of the craters that
cover the moon formed
when debris struck the
moon between 3.9 and
3.8 billion years ago
(BYA).
THE MOONS
SURFACE
THE LUNAR
ANATOMY
 The
dark and light patches on the full moon’s surface
reveal the bright mountains, dark plains, and thousands of
giant craters that tell of a long history of violent impacts.
 Aristotle
(322 B.C.)
suggested an Earthcentered, or
geocentric, model of
the solar system.
 In
this model, the sun,
the stars, and the
planets revolved
around Earth.
GEOCENTRIC MODEL
OF THE SOLAR SYSTEM
 The
major problem
with a geocentric
model is that it does
not explain the
retrograde motion of
the planets in our
night sky.
EPICYCLES MODELS
OF THE SOLAR
SYSTEM
 Ptolemy
(168 A.D.)
theorized that
planets most move
in small circles,
called epicycles, as
they revolved in
larger circles around
Earth.
EPICYCLES MODELS
OF THE SOLAR
SYSTEM
 This
model made
some sense and the
astronomical
predictions of
Ptolemy's geocentric
model were used to
prepare astrological
charts for over 1500
years.
EPICYCLES MODELS
OF THE SOLAR
SYSTEM
CHECK FOR UNDERSTANDING
 What
is the Geocentric Model of the
solar system and who created it?
 What
does epicycles refer to?
 What
is the anatomy of the moon?

In 1543, the geocentric
system met its first serious
challenge with the
publication of Copernicus’
‘De revolutionibus orbium
coelestium’, which
suggested that the Earth
and the other planets
instead revolved around the
Sun.

Aristarchos (230 BC), was
a Greek mathematician,
presented the first
known heliocentric model of
the solar system.
HELIOCENTRIC
MODELS OF THE
SOLAR SYSTEM
HELIOCENTRIC
MODELS OF THE
SOLAR SYSTEM
 Despite
Copernicus’s convincing work, the geocentric
model does not go away quickly.
 With
the Invention of the telescope 1609, Galileo made
observations of Jupiter’s moons which also called into
question some of the tenets of geocentrism but his work
alone did not seriously threaten it.
HELIOCENTRI
C- TURNING
THE TIDE
Kepler
 As
the telescope becomes more accessible and
refined (better) Galileo’s work along with: Kepler, Brahe,
Cassini and Huygens were finally enough to turn the tide
of the skeptics.
 Sir
Isaac Newton would
be born the same day
Galileo died.
 In
the 1700’s Newton’s laws of
motion, when
combined with his law
of gravity and Kepler’s
elliptical orbit theory,
successfully explained
all motions of
astronomical bodies for
the next 200 years.
HELIOCENTRICTURNING THE TIDE
 In
1758 the Catholic
Church dropped the
general prohibition of
books advocating
heliocentrism from
the Index of Forbidden
Books.
 In
1822 Pope Pius
VII approved a decree
by the Sacred
Congregation of the
Inquisition to allow the
printing of heliocentric
books in Rome.
OPPOSITION TO HELIOCENTRISM WANES
CHECK FOR UNDERSTANDING

What is the Heliocentric Model of the solar system
and who created it?

What significant findings did Newton and Kepler
discover?
LAND
TELESCOPES
 Telescopes
 The
Chile’s Atacama Desert
have come a long way since Galileo.
European Southern Observatory is planning to build a
telescope in Chile that will be almost half the length of a
soccer field in diameter and gather 15 times more light
than the largest optical telescopes operating today.
LAND
TELESCOPES
 Here
in L.A we have the Griffith Observatory which allows
the entrance to the general public for a fee – of course.
 While
land telescopes are more accessible, space
telescopes have the advantage of no atmospheric
interference (weather, dust, smog).
HUBBLE
SPACE
TELESCOPE

The Hubble Space Telescope was developed NASA and
deployed from shuttle Discovery, STS-31 April 25, 1990.

Hubble’s domain extends from the ultraviolet, through the
visible (to which our eyes are sensitive), and to the nearinfrared.
HUBBLE
DEEP
FIELD
www.spacetechnology.com
 Developed
by Cal Tech
in Pasadena and
operated by JPL, the
NASA Spitzer Space
Telescope is designed
to detect infrared
images.
 It
was launched by
Delta II rocket Aug. 25,
2003.
SPITZER SPACE
TELESCOPE
SPITZER
MESSIER
95
CHANDRA
SPACE
TELESCOPE
 Launched
 NASA's
July 23, 2003 STS 93–Shuttle Columbia
Chandra X-ray Observatory is designed to
detect X-ray emission from very hot regions of the
universe such as exploded stars, clusters of galaxies, and
matter around black holes.
CHAND
RA
M84
PAST, PRESENT AND FUTURE OF SPACE
TELESCOPES
JAMES WEBB SPACE TELESCOPE (JWST)

The James Webb Space Telescope is an orbiting infrared
observatory that will complement and extend the discoveries of
the Hubble Space Telescope, with longer wavelength coverage
and greatly improved sensitivity.
WHERE WILL THE JWST ORBIT