TEST BANK 21ST CENTURY
ASTRONOMY THE SOLAR SYSTEM 5TH EDITION BY KAY
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Chapter 14: Our Star—The
Sun
Learning
Objectives
Define the boldfaced vocabulary terms within the chapter.
14.1 The Sun Is Powered by Nuclear Fusion
Describe hydrostatic equilibrium.
Multiple Choice: 3, 4, 5, 6, 7
Short Answer: 1, 2
Relate how a change in internal characteristics of a star
(e.g., core temperature, energy generation) will change its surface
characteristics (e.g., surface temperature, luminosity, size).
Multiple Choice: 15
Short Answer: 7
Illustrate the process of nuclear fusion between two nuclei.
Multiple Choice: 8, 10, 13, 14, 21
Explain why nuclear fusion is able to generate energy.
Multiple Choice: 1, 2, 9
Describe the conditions needed for nuclear fusion to occur.
Multiple Choice: 11, 18, 19, 20
Short Answer: 5
Illustrate the steps by which hydrogen nuclei are fused into
helium in the Sun in the proton-proton chain.
Multiple Choice: 12
Short Answer: 6
14.2 Energy Is Transferred from the
Interior of the Sun
Compare and contrast the conditions under which energy in the
sun is transported by radiation and by convection.
Multiple Choice: 24, 25, 26, 27, 28, 31
Short Answer: 8, 9, 11
Describe how opacity affects the speed at which energy is
radiated out of the Sun.
Multiple Choice: 22, 23, 29, 30, 32
Discuss how neutrino detection was used to test our theory of
nuclear fusion in the Sun, and how that led to a better understanding of
neutrinos themselves.
Multiple Choice: 33, 36, 37
Short Answer: 10, 13
Summarize the solar-neutrino problem and solution.
Multiple Choice: 34, 38
Short Answer: 12
Explain how helioseismology has been used to probe the
structure of the Sun.
Multiple Choice: 35, 39, 40
Short Answer: 14
14.3 The Atmosphere of the Sun
Illustrate the effect of limb darkening.
Multiple Choice: 41, 42
Short Answer: 15
Determine why sunlight has an absorption spectrum even though
we treat it as a blackbody.
Multiple Choice: 44, 45
Short Answer: 17
Characterize the different layers of the solar atmosphere.
Multiple Choice: 43, 46, 47, 48, 49, 50, 51, 52
Short Answer: 16, 18
14.4 The Atmosphere of the Sun Is Very Active
Describe how magnetic effects in the sun create its solar
activity.
Multiple Choice: 53, 55, 57, 58, 60, 61, 62, 63, 66
Short Answer: 19, 21, 28
Summarize our theory explaining the sunspot cycle.
Multiple Choice: 56, 64, 65, 68
Short Answer: 22
Characterize the extent to which solar activity creates
measurable effects on Earth.
Multiple Choice: 54, 67, 69, 70
Short Answer: 23, 24, 25, 26, 27, 29, 30
Working It Out 14.1
Compute the fusion rate of a star.
Multiple Choice: 16
Short Answer: 3
Relate the mass, luminosity, fuel consumption, and lifetime
of a star powered by nuclear fusion.
Multiple Choice: 17
Short Answer: 4
Working It Out 14.2
Use the Stefan-Boltzmann law to compare the temperature and
flux of a star’s surface to its sunspots.
Short Answer: 20
MULTIPLE CHOICE
1.
The Sun is not
responsible for which of the following?
a.
daylight
b.
plant photosynthesis
c.
weather
d.
plate tectonics
2.
The Sun has a mass of
a.
2 × 1010
kg.
b.
2 × 1025
kg.
c.
2 × 1030
kg.
d.
2 × 1035
kg.
e.
2 × 1045
kg.
3.
Hydrostatic equilibrium
is a balance between
a.
heat and centrifugal
force.
b.
core temperature and
surface temperature.
c.
pressure and gravity.
d.
radiation and heat.
e.
centrifugal force and
gravity.
4.
Where does hydrostatic
equilibrium exist in the Sun?
a.
only in the core, where
energy production via fusion can balance gravity
b.
in the outer layers of
the atmosphere, where most of the visible light is produced
c.
just outside the core,
where heat from nuclear fusion is transported outward
d.
throughout the Sun
5.
Density, temperature,
and pressure increase as you move inward in the interior of the Sun. This means
that the weight of the star pushing inward at a given radius _________ as you
move inward toward the core.
a.
increases
b.
decreases
c.
stays the same
d.
There is not enough
information to answer.
6.
Which of the curves in
the figure shown below best matches the shape of a graph of the density of
material inside the Sun (in thousands of kg/m3) as you move farther
away from the center?
a.
A
b.
B
c.
C
d.
D
e.
E
7.
The balance of energy
in the solar interior means that
a.
energy production rate
in the core equals the rate of radiation escaping the Sun’s surface.
b.
the source of energy in
the core is stable and will sustain the Sun for millions of years.
c.
the outer layers of the
Sun absorb and re-emit the radiation from the core at increasingly longer
wavelengths.
d.
radiation pressure
balances the weight of the overlying solar layers.
e.
the core of the Sun has
pressure that is higher than that of the outer layers.
8.
Which force is
responsible for holding the protons and neutrons in the nucleus of an atom
together?
a.
gravity
b.
strong nuclear force
c.
electric force
d.
magnetic force
e.
electrons pushing them
together
9.
The majority of the
Sun’s energy comes from
a.
gravitational
contraction.
b.
nuclear fission of
uranium.
c.
hydrogen fusion.
d.
helium burning.
e.
burning material as in
a fire.
10.
Nuclei of atoms are
held together by
a.
gravity.
b.
the electric force.
c.
the strong nuclear
force.
d.
the weak nuclear force.
11.
What is the approximate
temperature at the center of the Sun?
a.
106 K
b.
1.5 × 107 K
c.
2.5 × 107 K
d.
10,000 K
12.
The net result of the
proton-proton chain of nuclear reactions is that four protons are converted
into
a.
one helium nucleus as
well as energy, electrons, and neutrinos.
b.
one helium nucleus as
well as deuterium, electrons, and energy.
c.
one helium nucleus, as
well as energy, positrons, and neutrinos.
d.
two helium nuclei, as
well as neutrinos and positrons.
13.
What do astronomers
mean when they say that the Sun makes energy by hydrogen burning?
a.
The Sun is combusting
hydrogen in a fire and releasing energy.
b.
The Sun is fusing
hydrogen into uranium and releasing energy.
c.
The Sun is made of
mostly hydrogen at very high temperature.
d.
The Sun is fusing
hydrogen into helium and releasing energy.
e.
The Sun is accumulating
hydrogen from the solar wind and releasing energy.
14.
When two atomic nuclei
come together to form a new species of atom, this is called
a.
nuclear fission.
b.
nuclear recombination.
c.
nuclear splitting.
d.
nuclear fusion.
e.
ionization.
15.
Suppose by some
mysterious process that the nuclear fusion rate in the core of the Sun were to
increase. What would happen to the appearance of the Sun?
a.
It would shrink so that
the higher gravity could balance the increased pressure from the core.
b.
It would grow larger
and hotter, making it more luminous.
c.
It would grow larger
but stay at the same temperature, making it more luminous.
d.
It would grow larger
but cooler.
16.
If the Sun converts 5 × 1011
kg of H to He per second and the mass of a single hydrogen nucleus is 1.7 × 10−27 kg, how many net
proton-proton reactions go on per second in the Sun? What is the luminosity
produced if the mass difference between a single helium nucleus and four
hydrogen nuclei is 4 × 10_29 kg? Note that 1 Watt = 1 m2
kg/s3.
a.
7 × 1037
reactions per sec; 4 × 1026 Watt
b.
3 × 1038
reactions per sec; 1027 Watt
c.
3 × 1038
reactions per sec; 4 × 1026 Watt
d.
7 × 1037
reactions per sec; 5 × 1025 Watt
e.
3 × 1037
reactions per sec; 6 × 1024 Watt
17.
If the Sun converts 5 × 1011
kg of H to He per second and 10 percent of the Sun’s total mass is available
for nuclear burning, how long might we expect the Sun to live?
a.
104 years
b.
108 years
c.
1010 years
d.
1011 years
e.
1014 years
18.
If the core of the Sun
were hotter than it is now, how would the Sun’s energy production change?
a.
It would produce less
energy per second than it does now.
b.
It would produce more
energy per second than it does now.
c.
Its energy production
would vary more than it does now.
d.
Its energy production
would be more stable than it is now.
e.
The Sun’s energy
production would not change.
19.
The energy that fuels
the Sun is generated
a.
only on its surface.
b.
only in its core.
c.
only in the solar wind.
d.
both in its core and on
its surface.
e.
in its core, on its
surface, and in the solar wind.
20.
Why is hydrogen burning
the main energy source for main-sequence stars?
a.
Hydrogen is the most
common element in stars.
b.
Hydrogen nuclei have
the smallest positive charge.
c.
Hydrogen burning is the
most efficient of all fusion or fission reactions.
d.
Hydrogen can fuse at
temperatures lower than other elements.
e.
All the above are valid
reasons.
21.
The net effect of the
proton-proton chain is that four hydrogen nuclei are converted to one helium
nucleus and _________ are released.
a.
visible wavelength
photons
b.
gamma ray photons,
positrons, and neutrinos
c.
ultraviolet photons and
neutrinos
d.
X-ray photons,
electrons, and neutrinos
e.
infrared photons and
positrons
22.
In the radiative zone
inside the Sun, photons are transported from the core to the convective zone
over a time of
a.
many thousands of
years.
b.
many millions of years.
c.
seconds.
d.
a few hours.
e.
months.
23.
If the Sun stopped
nuclear fusion in its core, how long would it take for its luminosity to change
significantly?
a.
months
b.
a few hours
c.
seconds
d.
about 100,000 years
24.
Which of the following
method(s) is (are) not used to transport energy from the core of the Sun
to its surface?
a.
radiation
b.
convection
c.
conduction
d.
All of the above are
important in the solar interior.
e.
None of the above are
important in the solar interior.
25.
If you hold onto one
end of a metal spoon after placing the other end in a pot of boiling water, you
will burn your hand. This is an example of energy being transported by
a.
radiation.
b.
convection.
c.
conduction.
d.
convection and
radiation.
e.
radiation and
conduction.
26.
Some restaurants place
food under infrared heat lamps so that it stays warm after it has been cooked.
This is an example of energy being transported by
a.
radiation.
b.
convection.
c.
conduction.
d.
convection and
conduction.
e.
radiation and
conduction.
27.
The interior zones of
the Sun are distinguished by
a.
jumps in density
between zones.
b.
their temperature
profiles.
c.
pressure differences
inside each zone.
d.
their modes of energy
transport.
e.
all of the above
28.
Which of the following
layers of the Sun makes up the majority of its interior?
a.
the core
b.
the radiative zone
c.
the convective zone
d.
the photosphere
e.
the chromosphere
29.
Approximately how long
does it take the photons released in nuclear reactions in the core of the Sun
to exit the Sun?
a.
8 minutes
b.
16 hours
c.
1,000 years
d.
100,000 years
e.
4.6 billion years
30.
Light from the Sun
reaches Earth approximately _________ times faster than photons released in
fusion in the core.
a.
1,000
b.
600,000
c.
1 million
d.
6 billion
e.
10 billion
31.
When you turn on the
heater in a car, the passengers in the front seat warm up first, and then
eventually the warm air gets to the passengers in the back seat. This is an
example of energy being transported by
a.
radiation.
b.
convection.
c.
conduction.
d.
convection and
conduction.
e.
radiation and
conduction.
32.
Which of these can
travel directly from the center of the Sun to Earth in about 8 minutes?
a.
photons
b.
electrons
c.
protons
d.
neutrons
e.
neutrinos
33.
What makes neutrinos so
different from other particles of matter?
a.
They interact very
weakly with other particles.
b.
They interact very
strongly with other particles.
c.
They are the only
particles that move quickly.
d.
They move very slowly.
34.
How was the solar
neutrino problem solved?
a.
by postulating that
neutrinos have a very large mass
b.
by postulating that
neutrinos oscillate between three different types
c.
by postulating that
some neutrinos become photons during their journey
d.
by postulating that
some neutrinos interact more strongly with matter such that they are absorbed
locally inside the Sun
35.
How does the fact that
the surface of the Sun rings like a bell help us better understand the Sun?
a.
The ringing tells us
how quickly the Sun is expanding with time.
b.
The ringing helps us
understand the solar interior better.
c.
The ringing reveals how
rapidly the Sun’s magnetic field is changing.
d.
The ringing helps us
determine the surface temperature of the Sun.
36.
The detection of solar
neutrinos confirms that
a.
the Sun’s core is
powered by proton-proton fusion.
b.
energy transport by
radiation occurs throughout much of the solar interior.
c.
magnetic fields are
responsible for surface activity on the Sun.
d.
convection churns the
base of the solar atmosphere.
e.
sunspots are cooler
than the rest of the photosphere.
37.
If neutrinos oscillated
between five different types of neutrino during their transit from the Sun to
Earth and we could only detect one type of neutrino, then how many neutrinos
would we have detected compared with what was emitted by the Sun?
a.
one-half as many
b.
one-third as many
c.
one-fourth as many
d.
one-fifth as many
e.
We would detect no
neutrinos.
38.
The solar neutrino
problem was solved by
a.
adjusting the rate of
hydrogen burning in solar models.
b.
improving detector efficiencies
so more neutrinos were observed.
c.
postulating that
neutrinos had mass and oscillated between three different types.
d.
lowering the percentage
of helium in models of solar composition.
e.
correctly measuring the
density of the Sun’s interior.
39.
By studying how the
surface of the Sun vibrates like a struck bell we can determine its
a.
age.
b.
interior density.
c.
total mass.
d.
size.
e.
temperature.
40.
We can determine how
the density changes with radius in the Sun using
a.
radar observations.
b.
neutrino detections.
c.
high-energy (gamma ray)
observations.
d.
helioseismology.
e.
infrared observations.
41.
The surface of the Sun
appears sharp when we look at it in visible light because
a.
the photosphere is
cooler than the layers below it.
b.
the photosphere is thin
compared with the other layers in the Sun.
c.
the photosphere is much
less dense than the convection zone.
d.
the photosphere is
transparent to radiation.
e.
the Sun has a distinct
surface.
42.
Imagine that you
observed the Sun and measured the brightness of the face of the Sun at the
locations marked in the figure below. At which of these locations would you
measure the lowest brightness?
a.
A
b.
B
c.
C
d.
D
e.
They would all have the
same brightness.
43.
The hottest layer of
the solar atmosphere is the
a.
outer convection zone.
b.
photosphere.
c.
chromosphere.
d.
corona.
44.
The solar spectrum is
an example of a(n) _________ spectrum.
a.
emission
b.
absorption
c.
continuum
d.
blackbody
e.
X-ray
45.
Which of the following cannot
be measured from the optical absorption spectrum of the Sun?
a.
the temperature of the
photosphere
b.
the composition of the
Sun
c.
the temperature of the
corona
d.
the density of the
photosphere
46.
The Sun’s chromosphere
appears red because
a.
it is hotter than the
photosphere.
b.
as the Sun rotates, the
chromosphere appears to move away from us radially.
c.
it has a higher
concentration of heavy metals.
d.
it is made of mostly
helium.
e.
its spectrum is
dominated by Hα emission.
47.
The figure below shows
the Sun during a solar eclipse at visible wavelengths. Which part of the Sun is
visible around the shadow of the Moon?
a.
chromosphere
b.
photosphere
c.
radiative zone
d.
convective zone
e.
corona
48.
The best wavelength to
use to observe a solar prominence is
a.
550 nm, green visible
light.
b.
656 nm, a red hydrogen
emission line.
c.
16 mm, an ultraviolet
emission line.
d.
21 cm, microwave
emission.
e.
0.02 nm, X-ray
emission.
49.
The Sun’s corona has a
temperature of approximately 1 million degrees. At what wavelength and in what
part of the electromagnetic spectrum does its radiation peak?
a.
550 nm, visible
b.
2 × 10_5
m, infrared
c.
4 × 10_7
m, ultraviolet
d.
3 × 10_9
m, X-rays
e.
6 m, radio
50.
Which of the layers of
the Sun is located the farthest from the center of the Sun?
a.
chromosphere
b.
photosphere
c.
radiative zone
d.
convective zone
e.
corona
51.
We know the Sun’s
corona is very hot because
a.
we observe it emitting
radiation at visible wavelengths.
b.
the chromosphere and
the photosphere are that hot, too.
c.
we observe absorption
from highly ionized atoms of iron and calcium in its spectrum.
d.
the gas emits most of
its radiation at radio wavelengths.
e.
all of the above
52.
Suppose coronal holes
covered a larger fraction of the Sun’s surface than they currently do. Which of
the following consequences would result?
a.
The solar wind would
contain a higher density of particles.
b.
The solar wind would
become hotter.
c.
The solar wind would
move faster.
d.
The composition of the
solar wind would change.
53.
What keeps the gas in
the Sun’s corona from flying away from the Sun?
a.
gravity
b.
strong nuclear force
c.
the Sun’s magnetic
field
d.
the solar wind
e.
sunspots
54.
Which of the following
is not a result of an increase in solar activity?
a.
The altitudes of
orbiting satellites decrease.
b.
Airplanes have trouble
navigating.
c.
Stronger auroras are
seen.
d.
Power grids can be
damaged.
e.
None of the above; all
of these are caused by increased solar activity.
55.
The figure shown below,
taken at visible wavelengths, shows a section of the Sun with sunspots visible.
Which of the labeled regions is the lowest temperature?
a.
region A
b.
region B
c.
region C
d.
They are all the same
temperature.
e.
There is not enough
information to determine their relative temperatures.
56.
In a sunspot, the umbra
is
a.
hotter than the
penumbra.
b.
cooler than the
penumbra.
c.
the same temperature as
the penumbra.
d.
less dense than the
penumbra.
57.
The solar magnetic
field
a.
returns to the same
polarity every 11 years.
b.
switches polarity every
22 years.
c.
switches polarity every
11 years.
d.
retains the same
polarity during the entire solar activity cycle.
58.
Sunspots appear dark
because they have _________ than those of the surrounding gases.
a.
densities that are
higher
b.
densities that are
lower
c.
pressures that are
higher
d.
temperatures that are
lower
e.
temperatures that are
higher
59.
If a sunspot appears
one-quarter as bright as the surrounding photosphere, and the average
temperature of the photosphere is 5800 K, what is the temperature of the gas in
this sunspot?
a.
3625 K
b.
4100 K
c.
4500 K
d.
5200 K
e.
5500 K
60.
Which of the following
are created by solar magnetic activity?
a.
sunspots
b.
prominences
c.
coronal mass ejections
d.
solar flares
e.
all of the above
61.
The darkest part of a
sunspot is called the
a.
penumbra.
b.
umbra.
c.
granule.
d.
photosphere.
e.
magnetic field.
62.
The magnetic field of
the Sun is continuously produced and deformed by
a.
its differential
rotation.
b.
the solar wind.
c.
changes in the rate of
nuclear fusion in the core.
d.
a liquid conducting
layer in the interior.
e.
This is a trick
question. The solar magnetic field is primordial.
63.
The Sun’s internal
magnetic field becomes tangled up over time because of
a.
coronal holes.
b.
coronal mass ejections.
c.
differential rotation.
d.
temperature changes in
the Sun’s core.
e.
all of the above
64.
If you observe a
maximum number of sunspots right now, how long would you have to wait to see
the next solar maximum?
a.
24 hours
b.
6 months
c.
1 year
d.
11 years
e.
22 years
65.
The Maunder Minimum was
a 60-year period when
a.
debris from a comet
collision blanketed the Sun.
b.
almost no sunspots
occurred on the Sun.
c.
the Voyager 2
spacecraft traversed the heliopause.
d.
very few dust storms
occurred on Mars.
e.
very few volcanic
eruptions occurred on Mars.
66.
The Sun’s magnetic
field reverses direction every
a.
24 hours.
b.
27 days.
c.
12 months.
d.
11 years.
e.
22 years.
67.
If a coronal mass
ejection occurs on the Sun that expels material at a speed of 800 km/s, how
long will it take these charged particles to reach the Earth?
a.
0.7 day
b.
1.4 days
c.
1.8 days
d.
2.2 days
e.
3.5 days
68.
When is the Sun most
luminous?
a.
when there are a
maximum number of sunspots
b.
when there are an
average number of sunspots
c.
when there are a
minimum number of sunspots
d.
The Sun’s luminosity
does not change.
e.
The Sun’s luminosity
changes, but it has no relation to the number of sunspots.
69.
When solar activity is
very high, the Earth’s atmosphere will
a.
expand.
b.
contract.
c.
remain approximately
the same.
d.
repel charged
particles.
e.
block out sunlight.
70.
Solar wind particles
hit the surface of the Moon, but they don’t make it to the surface of the Earth
because the Earth
a.
is larger than the
Moon.
b.
is warmer than the
Moon.
c.
has an atmosphere while
the Moon does not.
d.
has a magnetic field
while the Moon does not.
e.
is farther from the Sun
than the Moon is.
SHORT ANSWER
1.
In addition to the laws
of physics and chemistry, what information do we need to know about our Sun to
calculate its internal structure and radius?
2.
Explain why hydrostatic
equilibrium results in the center of the Sun having the highest pressure and
temperature.
3.
Calculate the amount of
energy released by converting four hydrogen atoms into one helium atom. The
mass of a hydrogen atom is 1.67 × 10_24g;
the mass of a helium atom is 6.65 × 10_24
g. The speed of light is 3 × 108 m/s.
4.
Through hydrogen
fusion, the Sun loses approximately 4 million tons of mass each second. If it
burns hydrogen at this rate for 10 billion years, what percentage of its
original mass will it lose in all? (Note: The mass of the Sun is 1.99 × 1030
kg, and 1 ton = 1,000 kg.)
5.
Why is hydrogen burning
the main energy source for main-sequence stars? Give at least two reasons.
6.
In the proton-proton
chain, the net reaction is that 4 protons are converted into 1 helium nucleus.
What other byproducts are released in this reaction, and why?
7.
In the text we
considered the case of a “too-large” Sun. Show that a star with the same mass,
composition, radius, and luminosity as the Sun, but with a higher temperature
(that is, a “too-hot” Sun), also leads to a contradiction.
8.
List three methods of
energy transport in nature and explain how the energy is being transferred in
each of those methods. Which two are means by which energy is transported
inside the Sun?
9.
The figure below shows
a diagram of the Sun with zones labeled A, B, and C. Explain how energy is
being transferred in each of the three regions.
10.
Explain why the
solution to the solar neutrino problem is an excellent example of how
observations drive the evolution of science.
11.
Explain why the
radiative zone in the solar interior gives way to a convective zone
approximately two-thirds of the way to the surface.
12.
Describe the solar
neutrino problem and its solution.
13.
Why are neutrino
detectors located deep underground?
14.
Describe how
helioseismologists measure the opacity of the solar interior.
15.
What is “limb
darkening”? Explain why limb darkening occurs in the Sun.
16.
What makes the
chromosphere appear so red?
17.
What is the origin of
the absorption lines in the Sun’s spectrum?
18.
The temperature profile
of the solar atmosphere is shown in the figure shown below. What causes the
sharp increase in temperature when going from the chromosphere to the corona?
19.
Explain why magnetic
fields trap coronal gas over much of the solar surface but allow it to escape
in coronal holes.
20.
If a sunspot is half as
bright as the surrounding photosphere of the Sun, what is the approximate
temperature of the gas in the sunspot if the photosphere’s average temperature
is 5800 K?
21.
The Sun exhibits
differential rotation. Explain what differential rotation is. Which planets
also do this? Why don’t the others?
22.
When, during its
11-year cycle, is the Sun most luminous? What might this have to do with the
Maunder Minimum?
23.
Astronauts in space
could be harmed by the high-energy particles given off during a solar flare.
So, when a solar flare is observed, a warning can be given to astronauts to
tell them to get inside the space station for protection. Explain why there is
enough time between the first observation of a flare and the arrival of the harmful
particles for this system to work.
24.
If a coronal mass
ejection occurred on the Sun and ejected particles toward the Earth that
traveled at the speed of 1,000 km/s, how long would it take them to reach
Earth?
25.
If the Sun went through
a period where there were many sunspots for a number of decades straight, what
would happen to the climate of the Earth?
26.
How do periods of
strong solar activity affect near-Earth-orbiting spacecraft?
27.
Why is there increased
drag on spacecraft orbiting the Earth during periods of increased solar
activity?
28.
When gas in a sunspot
cools, it does not sink into the solar interior as one would expect for
material in an atmosphere. Why?
29.
Explain what the
heliosphere is and how it helps protect life on Earth.
30.
What eventually stops
the solar wind from expanding in the outer reaches of our Solar System, 100 AU
from the Sun?
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