The_S0lar_System_9th.pdf

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Imagine the history of the Universe
as a time line down the middle of an
American football field. The story
begins on one goal line as the big
bang fills the Universe with energy
and a fantastically hot gas of
hydrogen and helium. Follow the
history from the first inch of the
time line as the expansion of
the Universe cools the gas
and it begins to form galaxies
and stars.
The Dark Age when
the big bang had
cooled and before
stars began to shine
Formation of the
first galaxies
well under way
The Age of Quasars: Galaxies,
including our home galaxy, actively
forming, colliding, and merging
The expansion of the
Universe stops slowing
and begins accelerating.
Goal
line
Recombination: A few hundred
thousand years after the big
bang, the gas becomes
transparent to light.
Anglo-Australian Observatory/David Malin Images
Th
e
First
Inch
One-
inch l
ine
A typical galaxy contains 100 billion stars.
Copyright 2016 Cengage Learning. All Rights Reserved. May not be copied, scanned, or duplicated, in whole or in part. Due to electronic rights, some third party content may be suppressed from the eBook and/or eChapter(s).
Editorial review has deemed that any suppressed content does not materially affect the overall learning experience. Cengage Learning reserves the right to remove additional content at any time if subsequent rights restrictions require it.
The Sun is an ordinary star.
he
Last
Inch
T
Nuclear reactions
make energy.
•
First hominids
••
Earth
Moon
One-
inch l
in e
Ten thousand years ago, on
the 0.0026 inch line, humans
begin building cities and
modern civilization begins.
Formation of the Sun and
planets from a cloud of
interstellar gas and dust
Life begins in
Earth’s oceans.
Cambrian explosion 540 million
years ago: Life in Earth’s oceans
becomes complex.
Life first emerges
onto the land.
Age of Dinosaurs
Over billions of years, generation
after generation of stars have lived
and died, cooking the hydrogen
and helium of the big bang into the
atoms of which you are made.
Study the last inch of the time line
to see the rise of human ancestors
and the origin of civilization. Only in
the last flicker of a moment on the
time line have humans begun to
understand the story.
Copyright 2016 Cengage Learning. All Rights Reserved. May not be copied, scanned, or duplicated, in whole or in part. Due to electronic rights, some third party content may be suppressed from the eBook and/or eChapter(s).
Editorial review has deemed that any suppressed content does not materially affect the overall learning experience. Cengage Learning reserves the right to remove additional content at any time if subsequent rights restrictions require it.
Goal
line
Copyright 2016 Cengage Learning. All Rights Reserved. May not be copied, scanned, or duplicated, in whole or in part. Due to electronic rights, some third party content may be suppressed from the eBook and/or eChapter(s).
Editorial review has deemed that any suppressed content does not materially affect the overall learning experience. Cengage Learning reserves the right to remove additional content at any time if subsequent rights restrictions require it.
O
O
10
6
B
B
A
A
F
F
G
G
K
K
M
M
10
0R
Rigel A
Deneb
10
00
R
Betelgeuse
Antares
Polaris
10
R
Alnilam
Adara
Spica A
10
4
1R
Spica B
Sup
ergia
nts
Canopus
–5
10
2
M
ai
n
Rigel B
se
qu
en
ce
0.1
L /L
R
Capella A
Capella B
Vega
Sirius A
Pollux
Altair
Procyon A
Arcturus
Mira
Aldebaran A
ts
ia
n
G
0
M
v
1
Sun
5
α
Centauri B
Aldebaran B
0.0
1R
10
–2
0.0
01
R
Sirius B
40 Eridani B
Wolf 1346
10
Wh
ite
10
–4
Note: Star sizes are not to scale.
30,000
30,000
20,000
20,000
dw
arf
s
Procyon B
Van Maanen’s Star
Wolf 486
Barnard’s Star
Red
dwarfs
10,000
10,000
Temperature (K)
5000
5000
3000
3000
2000
2000
The H–R diagram is the key to understanding stars, their birth, their long lives, and their
eventual deaths. Luminosity (
L
/
L
(
) refers to the total amount of energy that a star emits
in terms of the Sun’s luminosity, and the temperature refers to the temperature of its
surface. Together, the temperature and luminosity of a star locate it on the H–R diagram
and tell astronomers its radius, its family relationships with other stars, and a great
deal about its history and fate.
Copyright 2016 Cengage Learning. All Rights Reserved. May not be copied, scanned, or duplicated, in whole or in part. Due to electronic rights, some third party content may be suppressed from the eBook and/or eChapter(s).
Editorial review has deemed that any suppressed content does not materially affect the overall learning experience. Cengage Learning reserves the right to remove additional content at any time if subsequent rights restrictions require it.

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