TEST BANK 21ST CENTURY ASTRONOMY THE SOLAR SYSTEM 5TH EDITION BY KAY
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Chapter
7: The Birth and Evolution of Planetary Systems
Learning Objectives
Define the bold-faced vocabulary terms within the chapter.
Multiple Choice: 1, 2, 4, 8, 16, 17, 27, 28, 29, 42
Short Answer: 7.1 Planetary Systems Form
around a Star
Illustrate the nebular hypothesis for solar system formation.
Multiple Choice: 5
Short Answer: Describe how astronomers and geologists arrived
at the same conclusions about Earth’s origins from different pieces of
evidence.
Multiple Choice: 3
Short Answer7.2 The Solar System Began with
a Disk
Explain conservation of angular momentum.
Multiple Choice: 9, 11, 13
Short Answer: Illustrate how accretion disks transfer angular
momentum so that stars and planets can collapse.
Multiple Choice: 10, 12, 14, 15
Short Answer: Describe the formation sequence of
planetesimals in an accretion disk.
Multiple Choice: 6, 7
7.3 The Inner Disk and Outer Disk Formed
at Different Temperatures
Explain conservation of energy.
Multiple Choice: 18, 21
Use conservation of energy to argue why material falling on
an accretion disk heats the disk up.
Multiple Choice: 24, 25
Short Answer:
Distinguish between refractory and volatile materials.
Multiple Choice: 22
Short Answer: Relate the temperature of an accretion disk to
the presence of different types of materials (e.g. refractory, volatile,
organic, ice) within the disk.
Multiple Choice: 23, 26
Short Answer: Compare and contrast primary and secondary
atmospheres.
Multiple Choice: 19, 20
Short Answer: 7.4 The Formation of Our Solar
System
Compare and contrast terrestrial and giant planets.
Multiple Choice: 31, 40
Describe how planetesimals become planets.
Multiple Choice: 32, 33, 34, 35, 37, 38, 39
Short Answer:
Show how temperature differences in our accretion disk led to
the formation of terrestrial and giant planets.
Multiple Choice: 30, 36
7.5 Planetary Systems Are Common
Summarize the five methods that astronomers use to detect
extrasolar planets.
Multiple Choice: 41, 43, 44, 45, 46, 47, 48, 50, 51, 52, 55,
56, 57, 58, 59, 60, 61, 62, 63, 64, 65
Short Answer: Describe how planetary migration accounts for
hot Jupiters being located very close to their host stars.
Multiple Choice: 49, 53, 54
Short Answer:
Working It Out 7.1
Compute and compare orbital and spin angular momentum.
Multiple Choice: 66, 67, 68, 69
Short Answer: Working It Out 7.2
Use Kepler’s third law to calculate the size of a planet’s
orbit.
Working It Out 7.3
Estimate the size of a planet by considering how much of its
parent star’s light it occults.
Multiple Choice: 70
MULTIPLE CHOICE
1.
What is a protostar?
a.
a planet like Jupiter
b.
a hot star
c.
a large ball of gas not
yet hot enough at its core to be a star
d.
a large ball of gas too
hot at its core to be a star
e.
a star with too much
angular momentum
2.
What is a meteorite?
a.
a streak of light in
the sky
b.
a rock that fell to
Earth from space
c.
a fireball
d.
a volcanic rock
e.
an iron-rich rock
3.
What have astronomers
and geologists studied to arrive at the same conclusions about Earth’s origins?
a.
volcanism in the solar
system
b.
comets
c.
meteorites
d.
the Moon
e.
the oceans
4.
The icy planetesimals
that remain in the solar system today are called
a.
asteroids.
b.
moons.
c.
meteorites.
d.
comet nuclei.
5.
Which of the following
is not a characteristic of the early Solar System, based on current
observations?
a.
The early solar nebula
must have been flattened.
b.
The material from which
the planets formed was swirling about the Sun in the same average rotational
direction.
c.
The first objects to
form started out small and grew in size over time.
d.
The initial composition
of the solar nebula varied between its inner and outer regions.
e.
Temperatures decreased
with increasing distance from the Sun.
6.
The smallest grains of
dust stick together in an accretion disk by which force?
a.
gravitational force
b.
electrostatic force
c.
magnetic force
d.
quantum mechanical
force
e.
strong force
7.
In order for two clumps
of dust to stick together in an accretion disk, they must collide at roughly
a.
100 m/s.
b.
10 m/s.
c.
1 m/s.
d.
0.5 m/s.
e.
0.1 m/s or less.
8.
What is a planetesimal?
a.
bodies of ice and rock
100 meters or more in diameter
b.
bodies of ice and rock
10 meters or less in diameter
c.
bodies of ice and rock
about 1 meter in diameter
d.
another name for dwarf
planets
e.
planets that haven’t
cleared their orbits
9.
According to the
conservation of angular momentum, if an ice-skater who is spinning with her
arms out wide slowly pulls them close to her body, this will cause her to . . .
a.
spin faster.
b.
spin slower.
c.
maintain a constant
rate of spin.
d.
fall down.
10.
Approximately how much
mass was there in the protoplanetary disk out of which the planets formed,
compared to the mass of the Sun?
a.
50 percent
b.
25 percent
c.
10 percent
d.
5 percent
e.
< 1 percent
11.
In the figure shown
below, the direction of the disk’s rotation is indicated. What is the direction
of the protostellar Sun’s rotation?
a.
impossible to tell
b.
in the opposite
direction as the disk’s rotation
c.
in the same direction
as the disk’s rotation
d.
perpendicular to the
disk’s rotation
12.
Consider the figure
shown below. At which point in time does the collapsing cloud have the greatest
angular momentum?
a.
1
b.
2
c.
3
d.
1 and 2, because the
protostar has not yet formed
e.
The cloud has the same
angular momentum at each point in time.
13.
The fact that Jupiter’s
radius is contracting at a rate of 1 mm per year results in
a.
Jupiter’s rotation rate
slowing down with time.
b.
Jupiter’s shape being
noticeably oblate.
c.
Jupiter moving slightly
farther from the Sun with time.
d.
Jupiter radiating more
heat than it receives from the Sun.
e.
Jupiter having a strong
magnetic field.
14.
If a collapsing
interstellar cloud formed only a protostar without an accretion disk around it,
what would happen?
a.
The forming protostar
would be significantly less massive than it would have been otherwise.
b.
The forming protostar
would be rotating too fast to hold itself together.
c.
Only giant planets
would form around the protostar.
d.
Only terrestrial
planets would form around the protostar.
e.
More planets would form
around the protostar.
15.
Conservation of angular
momentum slows a cloud’s collapse
a.
equally in all
directions.
b.
only when the cloud is
not rotating initially.
c.
mostly along directions
perpendicular to the cloud’s axis of rotation.
d.
mostly at the poles
that lie along the cloud’s axis of rotation.
e.
to a complete stop.
16.
What is a primary
atmosphere?
a.
the atmospheres that
all planets have today
b.
the gas captured during
the planet’s formation
c.
the gas captured after
the planet’s formation
d.
the oxygen and nitrogen
in Earth’s atmosphere
e.
the gas closest to the
planet’s surface
17.
What is a secondary
atmosphere?
a.
the atmosphere that
escapes
b.
the gas captured during
the planet’s formation
c.
the gas farthest from
the surface
d.
the atmosphere that
remains after the planet has formed
e.
the gas closest to the
planet surface
18.
Consider four spheres
of equal mass and size. Which has the most potential energy?
a.
a sphere on the top
shelf of a bookshelf
b.
a sphere rolling on the
floor at the base of the bookshelf
c.
a sphere sitting at
rest on the floor at the base of the bookshelf
d.
a sphere on the middle
shelf of a bookshelf
e.
a sphere that fell from
the top shelf to the floor
.
19.
The atmosphere of which
of these Solar System bodies is primary, as opposed to secondary, in origin?
a.
Venus
b.
Earth
c.
Saturn’s moon Titan
d.
Saturn
e.
Mars
20.
The primary atmospheres
of the planets are made mostly of
a.
carbon and oxygen.
b.
hydrogen and helium.
c.
oxygen and nitrogen.
d.
iron and nickel.
e.
nitrogen and argon.
21.
When you push your
palms together and rub them back and forth, you are demonstrating one way of
converting _________ energy into _________ energy.
a.
potential; thermal
b.
kinetic; potential
c.
thermal; kinetic
d.
kinetic; thermal
e.
potential; total
22.
The solid form of a
volatile material is generally referred to as a(n)
a.
metal.
b.
silicate.
c.
ice.
d.
rock.
e.
refractory material.
23.
Based on the figure
shown below, which planet(s) is(are) most likely to have the largest fraction
of its(their) mass made of highly volatile materials such as methane and
ammonia?
a.
Venus, Earth, and Mars
b.
Earth
c.
Saturn
d.
Jupiter
e.
Uranus
24.
What happens to the
kinetic energy of gas as it falls toward and eventually hits the accretion disk
surrounding a protostar?
a.
It is immediately
converted into photons, giving off a flash of light on impact.
b.
It is converted into
thermal energy, heating the disk.
c.
It is converted into
potential energy as the gas plows through the disk and comes out the other
side.
d.
It becomes the kinetic
energy of the orbit of the gas in the accretion disk around the protostar.
e.
It disappears into
interstellar space.
25.
What sets the
temperature of the pocket of gas in a protoplanetary disk?
a.
its distance from the
forming star
b.
how much kinetic energy
was converted to heat
c.
how much radiation from
the forming star shines on the gas
d.
a combination of A, B,
and C
26.
Whether or not a planet
is composed mostly of rock or gas is set by
a.
its mass.
b.
its temperature.
c.
its distance from the
star when it formed.
d.
a combination of A, B,
and C
27.
Which of the following
is a terrestrial planet?
a.
Mercury
b.
Jupiter
c.
Venus
d.
both A and B
e.
both A and C
28.
Which of the following
is a giant planet?
a.
Mercury
b.
Jupiter
c.
Venus
d.
both A and B
e.
both A and C
29.
Which is the best
description of a moon?
a.
any small icy body in
the solar system
b.
any small rocky body in
the solar system
c.
any natural satellite
of a planet or asteroid
d.
a captured asteroid
e.
a captured comet
30.
What is the most
important factor in determining whether or not a planet will be rocky like
terrestrial planets or gaseous like giant planets?
a.
the time at which the
planet forms
b.
the planet’s radius
c.
the planet’s distance
from the Sun
d.
whether the planet has
moons
e.
the planet’s internal
temperature
31.
Why do the outer giant
planets have massive gaseous atmospheres of hydrogen and helium whereas the
inner planets do not?
a.
These gases were more
abundant in the outer regions of the accretion disk where the outer planets
formed.
b.
The outer planets grew
massive quickly enough to gravitationally hold on to these gases before the
solar wind dispersed the accretion disk.
c.
The inner planets are
made of rock.
d.
Frequent early
collisions by comets with the inner planets caused most of their original
atmospheres to dissipate.
32.
Comets and asteroids
are
a.
other names for moons
of the planets.
b.
primarily located
within 1 astronomical unit (AU) of the Sun.
c.
all more massive than
Earth’s Moon.
d.
material left over from
the formation of the planets.
e.
other names for
meteors.
33.
The Moon probably
formed
a.
out of a collision
between Earth and a Mars-sized object.
b.
when Earth’s gravity
captured a planetesimal.
c.
when the accretion disk
around Earth fragmented.
d.
when planetesimals
collided to form a more massive object.
e.
when a piece of Earth
broke off and entered orbit.
34.
What prevented the Moon
from maintaining any atmosphere with which it originally formed?
a.
It repeatedly collided
with planetesimals.
b.
It is too close to the
Sun.
c.
The solar wind blew it
away.
d.
It is not massive
enough.
e.
It is tidally locked to
Earth.
35.
Which of the following
is not considered evidence of cataclysmic impacts in the history of our
Solar System?
a.
Uranus is “tipped over”
so that it rotates on its side.
b.
Valles Marineris on
Mars is a huge scar, many times deeper than the Grand Canyon, which spans
one-fourth the circumference of the planet.
c.
Mercury has a crust
that has buckled on the opposite side of an impact crater.
d.
Mimas has a crater
whose diameter is roughly one-third of the Moon’s size.
e.
Mercury, Earth’s Moon,
and many other small bodies are covered with many impact craters.
36.
The difference in
composition between the giant planets and the terrestrial planets is most
likely caused by the fact that
a.
the giant planets are
much larger.
b.
only the terrestrial
planets have iron cores.
c.
the terrestrial planets
are closer to the Sun.
d.
the giant planets are
made mostly of carbon.
e.
only small differences
in chemical composition existed in the solar nebula.
37.
Two competing models of
the formation of giant gaseous planets suggest they form either from gas
accreting onto a rocky core or from
a.
fragmentation of the
accretion disk that surrounds the protostar.
b.
the merger of two large
planetesimals.
c.
planets stolen from
another nearby protostar.
d.
materials condensing out
of the solar wind.
e.
an eruption of material
from the protostar.
38.
Was it ever possible
(or is it currently possible) for Jupiter to become a star?
a.
Yes, it is in the
process of becoming a star in the near future.
b.
Yes, but it cooled off
before it could become a star.
c.
No, it would have to be
at least 13 times more massive.
d.
No, its composition is
too different from stars for it to become one.
e.
No, it used to be
massive enough, but the solar wind has blown off too much of its mass.
39.
How much material in an
accretion disk goes into forming the planets, moons, and smaller objects?
a.
most of it
b.
roughly half of it
c.
none; these objects
were not formed in the accretion disk
d.
a small amount of it
40.
Why do the terrestrial
planets have a much higher fraction of their mass in heavy chemical elements
(as opposed to lighter chemical elements) than the giant planets?
a.
Terrestrial planets are
low in mass and high in temperature, thus their lighter chemical elements
eventually escaped to the outer reaches of the Solar System.
b.
The heavier elements in
the forming solar nebula sank to the center of the Solar System, thus the inner
terrestrial planets formed mostly from heavy chemical elements.
c.
The giant planets were
more massive than terrestrial planets, and the giant planets preferentially
pulled the lighter elements from the inner to the outer Solar System.
d.
Terrestrial planets
formed much earlier than giant planets before the hydrogen and helium had a
chance to cool and condense onto them.
e.
Terrestrial planets are
colder and thus more massive chemical elements condensed on them than on the
giant planets.
41.
Which property of an
extrasolar planet cannot be determined using the Doppler effect?
a.
orbital period
b.
orbital distance
c.
orbital speed
d.
mass
e.
radius
42.
What is the habitable
zone?
a.
the distance from a
star where liquid water can exist
b.
the location on the sky
where planets can be found
c.
the distance from a
star where liquid can exist
d.
the distance from a
star where planets have oxygen in the atmosphere
e.
1 AU from any star
43.
Which method can be
used to determine the radius of an extrasolar planet?
a.
Doppler shift
b.
transit
c.
microlensing
d.
direct imaging
e.
none of the above
44.
Most planets currently
found around other stars are
a.
rocky in composition
like terrestrial planets.
b.
2 to 10 MEarth,
which is smaller than Neptune.
c.
2 to 10 MJupiter.
d.
located at distances
much larger than Jupiter’s distance from the Sun.
e.
similar in mass to
Earth.
45.
Which is not a
scientific goal of NASA’s Kepler mission?
a.
finding Earth-sized
planets
b.
finding rocky planets
c.
finding Earth-sized
planets that could have liquid water
d.
finding intelligent
life on other planets
e.
All the above are goals
of the Kepler mission
46.
Consider a star that is
more massive and hotter than the Sun. For such a star, the habitable zone would
a.
be located inside 1 AU.
b.
be located outside 1AU.
c.
not exist at any radii.
d.
exist at every radii.
47.
The Kepler mission is
designed to search for extrasolar planets using the _________ method.
a.
Doppler shift
b.
transit
c.
microlensing
d.
direct imaging
48.
Earth-sized planets
have been found using the _________ method(s).
a.
Doppler shift
b.
transit and Doppler
shift
c.
microlensing
d.
direct imaging
e.
transit
49.
Astronomers believe
that the “hot Jupiters” found orbiting other stars must have migrated inward
over time
a.
by slowly accreting
large amounts of gas and increasing their gravitational pull.
b.
by losing their gas
because of evaporation.
c.
by losing orbital
angular momentum.
d.
after colliding with
another planet.
e.
after a close encounter
between their star and another star.
50.
The borderline between
the most massive planet and the least massive brown dwarf occurs at
a.
4 Jupiter masses.
b.
13 Jupiter masses.
c.
120 Jupiter masses.
d.
80 Jupiter masses.
e.
45 Jupiter masses.
51.
Have astronomers
detected any Earth-sized planets around normal stars yet?
a.
Yes, the Kepler
spacecraft is just starting to find them.
b.
Yes, although the ones
detected lie much closer to their stars than we do to ours.
c.
Yes, although the ones
detected lie much farther from their stars than we do from ours.
d.
No, we do not have the
technology to detect such low-mass planets yet.
e.
No; although we have
the technology to detect low-mass planets, we haven’t found any others yet.
52.
Why have astronomers
using the radial velocity method found more Jupiter-sized planets at a distance
of 1 AU around other stars than Earth-sized planets?
a.
A Jupiter-sized planet
occults a larger area than an Earth-sized planet.
b.
A Jupiter-sized planet
exerts a larger gravitational force on the star than an Earth-sized planet, and
the Doppler shift of the star is larger.
c.
A Jupiter-sized planet
shines brighter than an Earth-sized planet.
d.
Earth-sized planets are
much rarer than Jupiter-sized planets.
e.
Actually, the planets
found at these distances all have been Earth-sized.
53.
When astronomers began
searching for extrasolar planets, they were surprised to discover Jupiter-sized
planets much closer than 1 AU from their parent stars. Why is this surprising?
a.
These planets must have
formed at larger radii where temperatures were cooler and then migrated inward.
b.
Jupiter-sized, rocky
planets were thought to be uncommon in other solar systems.
c.
These planets must be
the remnants of failed stars.
d.
Earth-like planets must
be rarer than Jupiter-sized planets in other solar systems.
e.
Jupiter-sized planets
so close to the star are different than in our Solar System.
54.
Which of the following
is false?
a.
Hundreds of extrasolar
planets have been discovered to date from radial velocity surveys.
b.
The most common types
of extrasolar planets found to date have masses 10 times the mass of Jupiter
and lie within 5 AU from their parent star.
c.
Some planetary systems
have been found that contain multiple planets.
d.
A star can brighten
significantly because of gravitational lensing when a planet that orbits it
passes directly in front of the star.
e.
The Kepler mission has
begun to find terrestrial planets similar in size to Earth.
55.
Astronomers have used
radial velocity monitoring to discover
a.
extrasolar planetary
systems that are similar to our own Solar System.
b.
Earth-sized planets
around other stars.
c.
Earth-sized planets at
distances of 10 AU from their parent stars.
d.
extrasolar planetary
systems that contain more than one planet.
e.
all of the above
56.
An observer located
outside our Solar System, who monitors the velocity of our Sun over time, will
find that the Sun’s velocity varies by ± 12 m/s over a period of 12 years, due
to
a.
Jupiter’s gravitational
pull.
b.
Earth’s gravitational
pull.
c.
variations in its
brightness.
d.
convection on the Sun’s
surface.
e.
the sunspot cycle.
57.
Detecting a planet
around another star using the transit method is difficult because the
a.
planet must pass
directly in front of the star.
b.
planet must have a
rocky composition.
c.
star must be very dim.
d.
star must be moving
with respect to us.
e.
planet’s orbital period
is usually longer than 1 month.
58.
In the figure below,
which of the dips in the brightness of the star is(are) caused by the transit
of the planet with the largest orbital period?
a.
A
b.
B
c.
C
d.
A and B
e.
B and C
59.
Figure 7.4 shows data
from the transit study of a star in which three different planets repeatedly
transit in front of the star (A, B, and C). Which dip is(are) caused by the
transit of the planet with the smallest radius?
a.
A
b.
B
c.
C
d.
A, B, and C
e.
impossible to tell from
these data
60.
Using the Doppler
effect data shown in the figure below, determine the approximate orbital period
of the extrasolar planet.
a.
1 year
b.
3 years
c.
6 years
d.
8 years
e.
12 years
61.
Using the Doppler
effect data for a particular star shown in Figure 7.5 and assuming the star is
about the same mass as our Sun, determine the approximate orbital distance of
its exoplanet.
a.
1.1 AU
b.
6.4 AU
c.
18 AU
d.
36 AU
e.
3.3 AU
62.
From the data shown in
Figure 7.5, which property of an extrasolar planet cannot be determined?
a.
orbital period
b.
orbital distance
c.
radius
d.
mass
e.
All of the above
properties can be determined.
63.
What is the best method
to detect Earth-sized exoplanets with the telescopes and instrumentation that
exist today?
a.
Doppler shift
b.
Transit
c.
Microlensing
d.
Direct imaging
.
64.
Which of the following
is false?
a.
The masses of
exoplanets can be determined using the radial velocity technique.
b.
Most of the exoplanets
detected to date have masses that are between 2 and 10 MEarth.
c.
Some exoplanets have
been found in the habitable zone around their stars.
d.
Using the transit
technique, the Kepler satellite has detected rocky planets.
e.
No images of exoplanets
have been obtained because they are too far away.
65.
In the figure shown
below, what can be directly measured from the information given?
a.
the mass of the planet
b.
percentage reduction in
light
c.
size of the planet
d.
orbital radius of the
planet
e.
distance of the star
66.
What is the ratio of
the orbital angular momentum of Earth compared to its spin angular momentum?
Note that Earth has a radius of 6 × 106 m, and 1 AU is 1.5 × 1011
m.
a.
1
b.
70
c.
640
d.
25,000
e.
4.3 ×
106
67.
What is the ratio of
the orbital angular momentum of Jupiter to its spin angular momentum? Jupiter’s
orbit has a semimajor axis of 5 AU and period of 12 years, and Jupiter has a
rotation period of 0.4 day and a radius of 70,000 km.
a.
650,000
b.
26,000
c.
920
d.
38
e.
4.5
68.
If an interstellar
cloud having a diameter of 1016 m and a rotation period of 1 million
years were to collapse to form a sphere that had the diameter of our Solar
System, approximately 40 AU, what would its rotation period be? Assume the
cloud’s total mass and angular momentum did not change.
a.
1 million years
b.
600 years
c.
1 year
d.
6 years
e.
4 months
69.
Consider a small parcel
of gas in the cloud out of which the Sun formed that initially was located in
the accretion disk at a distance of 10 AU from the Sun and rotating around it
with a speed of 10 km/s. If this parcel of gas eventually found its way to a
distance of 1 AU from the Sun without changing its orbital angular momentum,
what would be its new rotation speed?
a.
100 km/s
b.
0.1 km/s
c.
0.001 km/s
d.
10 km/s
e.
1,000 km/s
70.
If an astronomer on a
planet orbiting a nearby star observed the Sun when Neptune was transiting in
front of the Sun, how would the Sun’s brightness change? Note that the radius
of Neptune is 2.5 × 107 m.
a.
The Sun’s brightness
would decrease by 0.1 percent.
b.
The Sun’s brightness
would increase by 0.1 percent.
c.
The Sun’s brightness
would increase by 1 percent.
d.
The Sun’s brightness
would decrease by 1 percent.
e.
The Sun’s brightness
would not change at all.
SHORT ANSWER
1.
Explain the nebular
hypothesis, and describe two observations that support it.
2.
Explain why astronomers
believe that the formation of planets is a natural by-product of star
formation.
3.
How do meteorites tell
us about how the solar system formed?
4.
What does conservation
of angular momentum mean?
5.
What evidence do we
have that the accretion disk that formed the Solar System was initially much
more dense near its center?
6.
Explain why an
accretion disk forms around a protostar when an interstellar cloud collapses.
7.
What happens to a
slowly rotating cloud as it collapses to form a stellar system?
8.
What is the difference
between refractory and volatile materials?
9.
Explain why there are
significant amounts of methane and ammonia in the atmospheres of Uranus and
Neptune but not nearly as much in the atmospheres of Jupiter and Saturn.
10.
Why does an accretion
disk heat up?
11.
The primary atmosphere
of Earth consisted of what type of chemical elements and from where did it
originate? What chemical elements did the secondary atmosphere of Earth consist
of and from where did it originate?
12.
Explain the primary
reasons why the inner solar nebula was hotter than the outer solar nebula.
13.
Why did the terrestrial
planets lose their primary atmospheres?
14.
How do astronomers
explain the basic difference in composition between the inner planets and the
outer planets?
15.
Why did the
planetesimals in the asteroid belt never coalesce into a planet?
16.
Why might a newly
discovered comet contain clues to the composition of the early solar nebula?
17.
What are craters in the
solar system evidence of?
18.
How did the formation
of our Moon differ from the formation of the Galilean moons of Jupiter?
19.
Approximately how massive
are most of the extrasolar planets that have been discovered using the Doppler
effect, and which planet in our Solar System is similar in mass? Why is the
Doppler effect method more likely to find massive (rather than low-mass)
planets and planets that are close to their stars?
20.
Explain why most of the
extrasolar planets that astronomers first detected were so-called “hot
Jupiters.”
21.
Have any Earth-sized,
terrestrial, extrasolar planets been detected? If so, explain what method(s)
is(are) used.
22.
In addition to the
percentage reduction in light, is anything else needed to determine the size of
the transiting planet?
23.
Explain how astronomers
use the Doppler effect to detect the presence of extrasolar planets.
24.
What property of an
extrasolar planet can be determined directly from the Doppler effect data shown
in the figure below? What other properties of the planet can then be
determined?
25.
Briefly explain the
five different observational methods we use to detect extrasolar planets. How
many extrasolar planets have been discovered to date?
26.
What evidence do we
have that planetary systems are common in the universe?
27.
What is planet
migration?
28.
What are some
limitations of the radial velocity method of exoplanet detection?
29.
What are some
limitations of the transit method of exoplanet detection?
30.
Compare the orbital
angular momentum of Earth and Jupiter. Which is larger and by how much? (Note
that Jupiter’s mass is 318 times that of Earth, the semimajor axis of Jupiter’s
orbit is 5.2 AU, and Jupiter’s orbital period is 12 years.)
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