Evolution Of Low-mass Stars

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Our Place in the Universe
Patterns in the Skymotions of Earth
Laws of Motion
Light and Telescopes
The Formation of Stars and Planets
Terrestrial Worlds in the Inner Solar System
Atmospheres of Venus, Earth, and Mars
The Giant Planets
Small Bodies of the Solar System
Measuring the Stars
Our Star: The Sun
Evolution of Low-Mass Stars
Evolution of High-Mass Stars
The Expansion of Space
The Realm of the Galaxies
Our Galaxy: The Milky Way
Modern Cosmology and the Origin of Structure
Life in the Universe

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Question 1

Free

True/False

A 10 M_ star will evolve through the same phases as a 1 M_ star.

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True

False

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Question 2

Free

True/False

Stars evolve primarily because they run out of fuel in their cores.

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True

False

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Question 3

Free

True/False

The more massive a star,the more hydrogen it has to burn,and the longer its main-sequence lifetime will be.

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True

False

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Question 4

Free

True/False

If a main-sequence star's core temperature increased,fusion reaction rates would decrease because the protons would be moving faster.

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True

False

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Question 5

Free

True/False

The percent of hydrogen in the Sun's core today is roughly half of what it had originally.

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True

False

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Question 6

True/False

The Sun will become a red giant star in about 2 billion years.

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True

False

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Question 7

True/False

Pressure from degenerate electrons keeps the core of a red giant star from collapsing.

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True

False

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Question 8

True/False

Once the core of a low-mass main-sequence star runs out of hydrogen,fusion in the star stops until the core temperature is high enough for helium fusion to begin.

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True

False

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Question 9

True/False

When a star burns hydrogen in a shell,it will never produce as much energy (per unit time)as when it burns hydrogen in the core because the core has a higher temperature.

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True

False

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Question 10

True/False

A low-mass star that burns helium in its core and hydrogen in a shell is more luminous than a similar star that burns only hydrogen in a shell around a dead core.

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True

False

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Question 11

True/False

Stars with masses similar to the Sun can lose more than 30 percent of their mass before they become white dwarfs.

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True

False

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Question 12

True/False

A star like the Sun will eventually become an electron degenerate white dwarf star.

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True

False

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Question 13

True/False

We can determine the age of a star cluster by measuring the color of the reddest red giant stars in the cluster.

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True

False

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Question 14

True/False

Binary stars can evolve to become novae and supernovae because slight differences in mass can mean large differences in main-sequence lifetimes.

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True

False

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Question 15

True/False

A Type Ia supernova is as luminous as 10 billion Suns.

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True

False

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Question 16

Multiple Choice

The evolutionary cutoff between low- and high-mass stars occurs at approximately:

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0.5 M_

1 M_

4 M_

8 M_

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Question 17

Multiple Choice

What factor is most important in determining a star's position on the main sequence and subsequent evolution?

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Temperature

Pressure

Mass

Radius

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Question 18

Multiple Choice

A main-sequence star is unique because:

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hydrostatic equilibrium exists at all radii

energy transport occurs via convection throughout much of its interior

hydrogen burning occurs in its core

it emits strong surface winds

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Question 19

Multiple Choice

In stellar fusion the term "ash" refers to:

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dusty product of fire from oxidation occurring within the core of the star

the result of nuclear fusion that collects in the core

the result of nuclear fusion that collects in the outer layers of a star

dusty product of fire from oxidation occurring in the outer layers of the star

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Question 20

Multiple Choice

Which star spends the longest time as a main-sequence star?

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0.5 M_

1 M_

3 M_

10 M_

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Evolution Of Low-mass Stars

A 10 M star will evolve through the same phases as a 1 M star.

Stars evolve primarily because they run out of fuel in their cores.

The more massive a star,the more hydrogen it has to burn,and the longer its main-sequence lifetime will be.

If a main-sequence star's core temperature increased,fusion reaction rates would decrease because the protons would be moving faster.

The percent of hydrogen in the Sun's core today is roughly half of what it had originally.

The Sun will become a red giant star in about 2 billion years.

Pressure from degenerate electrons keeps the core of a red giant star from collapsing.

Once the core of a low-mass main-sequence star runs out of hydrogen,fusion in the star stops until the core temperature is high enough for helium fusion to begin.

When a star burns hydrogen in a shell,it will never produce as much energy (per unit time)as when it burns hydrogen in the core because the core has a higher temperature.

A low-mass star that burns helium in its core and hydrogen in a shell is more luminous than a similar star that burns only hydrogen in a shell around a dead core.

Stars with masses similar to the Sun can lose more than 30 percent of their mass before they become white dwarfs.

A star like the Sun will eventually become an electron degenerate white dwarf star.

We can determine the age of a star cluster by measuring the color of the reddest red giant stars in the cluster.

Binary stars can evolve to become novae and supernovae because slight differences in mass can mean large differences in main-sequence lifetimes.

A Type Ia supernova is as luminous as 10 billion Suns.

The evolutionary cutoff between low- and high-mass stars occurs at approximately:

What factor is most important in determining a star's position on the main sequence and subsequent evolution?

A main-sequence star is unique because:

In stellar fusion the term "ash" refers to:

Which star spends the longest time as a main-sequence star?

A 10 M_ star will evolve through the same phases as a 1 M_ star.