chapter 29: stars earth science geology, the environment and the universe

Chapter 29: StarsChapter 29: Stars

EARTH SCIENCEGeology, the Environment and the Universe

Section 29.1 The Sun

Section 29.2 Measuring the Stars

Section 29.3 Stellar Evolution

CHAPTER

29 Table Of Contents

Click a hyperlink to view the corresponding slides. Exit

Essential Questions

• What are the layers and features of the Sun?

• How is the process of energy production in the Sun explained?

• How are the three types of spectra defined?

SECTION29.1

The Sun

Review Vocabulary

• magnetic field: the portion of space near a magnetic or current-carrying body where magnetic forces can be detected

• The Sun contains most of the mass of the solar system and has many features typical of other stars.

The SunSECTION29.1

New Vocabulary

photosphere

chromosphere

corona

solar wind

sunspot

solar flare

prominence

fusion

fission

The SunSECTION29.1

• The Sun is the largest object in the solar system, in both diameter and mass. The Sun contains more than 99 percent of all the mass in the solar system. It should not be surprising, then, that the Sun’s mass affects the motions of the planets and other objects.

Properties of the Sun

The SunSECTION29.1

• The Sun’s average density is similar to the densities of the gas giant planets. Computer models show that the density in the center of the Sun is about 1.50 × 105 kg/m3.

The SunSECTION29.1

• The Sun’s interior is gaseous throughout because of its high temperature—about 1 × 107 K in the center. At this temperature, all of the gases are completely ionized. This means that the interior is composed only of atomic nuclei and electrons, in the state of matter known as plasma.

The SunSECTION29.1

Please click the image above to view the interactive table.

• The outer regions of the Sun’s atmosphere are organized into layers, like a planetary atmosphere separated into different levels, and each layer emits energy at wavelengths resulting from its temperature.

The SunSECTION29.1

The Sun’s Atmosphere

• The photosphere is the innermost layer of the Sun’s atmosphere and is also its visible surface. It has an effective temperature of 5800 K and is about 400 km thick.

Photosphere

The SunSECTION29.1

• Outside the photosphere is the chromosphere, which is approximately 2500 km thick and has an average temperature of 15,000 K.

• Usually, the chromosphere is visible only during a solar eclipse, but astronomers can use special filters to observe it when the Sun is not eclipsed.

Chromosphere

The SunSECTION29.1

• The outermost layer of the Sun’s atmosphere, called the corona, extends several million kilometers from the outside edge of the chromosphere and usually has a temperature of about 3 to 5 million K.

The SunSECTION29.1

Corona

• The density of the gas in the corona is very low, which explains why the corona is so dim. It can be seen only when the photosphere is blocked by either special instruments, as in a coronagraph, or by the Moon during an eclipse.

The SunSECTION29.1

Corona

• Gas flows outward from the corona at high speeds and forms the solar wind. As this wind of charged particles, called ions, flows outward through the entire solar system, it bathes each planet in a flood of particles.

The SunSECTION29.1

Solar wind

• Charged particles in the solar wind are deflected by Earth’s magnetic field and are trapped in two huge rings, called the Van Allen belts.

• The high-energy particles in these belts collide with gases in Earth’s atmosphere and cause the gases to give off light, called the aurora.

The SunSECTION29.1

Solar wind

• Some features of the Sun change over time in a process called solar activity, which includes fountains and loops of glowing gas. Some of this gas has structure—a certain order in both time and place—driven by magnetic fields.

The SunSECTION29.1

Solar Activity

• The Sun’s magnetic field disturbs the solar atmosphere periodically and causes new features to appear. A sunspot is a dark spot on the surface of the photosphere that typically lasts two months, occurs in pairs, and has a penumbra and an umbra.

The SunSECTION29.1

Solar Activity

The Sun’s magnetic field and sunspots

• Astronomers have observed that the number of sunspots changes from minimum to maximum and then back to minimum again in about 11 years. At this point, the Sun’s magnetic field reverses, so that the north magnetic pole becomes the south magnetic pole and vice versa.

The SunSECTION29.1

Solar Activity

Solar activity cycle

• Because sunspots are caused by magnetic fields, the polarities of sunspot pairs reverse when the Sun’s magnetic poles reverse. Therefore, when the polarity of the Sun’s magnetic field is taken into account, the length of the cycle doubles to 22 years.

The SunSECTION29.1

Solar Activity

Solar activity cycle

• Coronal holes are often located over sunspot groups. Coronal holes are areas of low density in the gas of the corona and are the main regions from which the particles that comprise the solar wind escape.

The SunSECTION29.1

Solar Activity

Other solar features

• Solar flares are violent eruptions of particles and radiation from the surface of the Sun. Highly active solar flares are associated with sunspots.

The SunSECTION29.1

Solar Activity

• A prominence is an arc of gas ejected from the chromosphere, or gas that condenses in the Sun’s inner corona and rains back to the surface. Prominences can reach temperatures over 50,000 K and are associated with sunspots.

The SunSECTION29.1

Solar Activity

• Fusion is the combination of lightweight atomic nuclei into heavier nuclei, such as hydrogen fusing into helium.

• This is the opposite of the process of fission, which is the splitting of heavy atomic nuclei into smaller, lighter nuclei, like uranium into lead.

The SunSECTION29.1

The Solar Interior

• In the core of the Sun, helium is a product of the process in which hydrogen nuclei fuse.

• The mass of the helium nucleus is less than the combined mass of the four hydrogen nuclei, which means that mass is lost during the process.

The SunSECTION29.1

The Solar Interior

Energy production in the Sun

• Albert Einstein’s special theory of relativity shows that mass and energy are equivalent, and that matter can be converted into energy and vice versa.

The SunSECTION29.1

The Solar Interior

• The relationship between mass and energy can be expressed as E = mc2, where E is energy measured in joules, m is the quantity of mass that is converted to energy measured in kilograms, and c is the speed of light measured in m/s.

The SunSECTION29.1

The Solar Interior

• Einstein’s special theory of relativity explains that the mass lost in the fusion of hydrogen to helium is converted to energy, which powers the Sun.

The SunSECTION29.1

The Solar Interior

• Energy in the Sun is transferred mostly by radiation from the core outward to about 75 percent of its radius. The outer layers transfer energy in convection currents.

The SunSECTION29.1

The Solar Interior

Energy transport

• As energy in the Sun moves outward, the temperature is reduced from a central value of about 1 × 107 K to its photospheric value of about 5800 K.

• A tiny fraction of the immense amount of solar energy eventually reaches Earth.

The SunSECTION29.1

The Solar Interior

Energy transport

• Above Earth’s atmosphere, 1354 J of solar energy is received in 1 m2/s (1354 W/m2). However, not all of this energy reaches the ground because some is absorbed and scattered by the atmosphere.

The SunSECTION29.1

The Solar Interior

Solar energy on Earth

• A spectrum (plural, spectra) is visible light arranged according to wavelengths. There are three types of spectra: continuous, emission, and absorption.

The SunSECTION29.1

Spectra

• A spectrum that has no breaks in it, such as the one produced when light from an ordinary bulb is shined through a prism, is called a continuous spectrum. A continuous spectrum can also be produced by a glowing solid or liquid, or by a highly compressed, glowing gas.

The SunSECTION29.1

Spectra

• The spectrum from a noncompressed gas contains bright lines at certain wavelengths. This is called an emission spectrum, and the lines are called emission lines. The wavelengths of the visible lines depend on the element being observed because each element has its own characteristic emission spectrum.

The SunSECTION29.1

Spectra

• A spectrum produced from the Sun’s light shows a series of dark bands. These dark spectral lines are caused by different chemical elements that absorb light at specific wavelengths. This is called an absorption spectrum, and the lines are called absorption lines.

The SunSECTION29.1

Spectra

• Using the lines of the absorption spectra like fingerprints, astronomers have identified the elements that compose the Sun. The Sun is composed primarily of hydrogen and helium with small amounts of other gases.

The SunSECTION29.1

Solar Composition

• The Sun’s composition represents that of the galaxy as a whole. Most stars have proportions of the elements similar to the Sun.

The SunSECTION29.1

Solar Composition

The Sun has used only about 3 percent of its hydrogen.

a. true

b. false

SECTION29.1

Section Check

Which is the visible surface of the Sun?

a. photosphere

b. corona

c. chromosphere

d. prominence

SECTION29.1

Section Check

a. prominence

b. solar flare

c. coronal hole

d. solar wind

What is formed by gas flowing outward at a high speed from the Sun’s corona?

SECTION29.1

Section Check

Essential Questions

• How are distances between stars measured?

• What is the difference between brightness and luminosity?

• What are the properties used to classify stars?

Measuring the StarsSECTION29.2

• Stellar classification is based on measurement of light spectra, temperature, and composition.

Review Vocabulary• wavelength: the distance from one point

on a wave to the next corresponding point

New Vocabulary

constellation

binary star

parsec

parallax

apparent magnitude

absolute magnitude

luminosity

Hertzsprung-Russell diagram

main sequence

• Long ago, many civilizations looked at the brightest stars and named groups of them after animals, mythological characters, or everyday objects. These groups of stars are called constellations.

• Today, astronomers group stars by the 88 constellations named by ancient peoples.

Patterns of Stars

• Some constellations are visible throughout the year, depending on the observer’s location. Constellations that appear to rotate around one of the poles are called circumpolar constellations. Ursa Major, which contains the Big Dipper, is a circumpolar constellation for most of the northern hemisphere.

SECTION29.2

Patterns of Stars

Measuring the Stars

• Unlike circumpolar constellations, the other constellations can be seen only at certain times of the year because of Earth’s changing position in its orbit around the Sun.

Patterns of Stars

• The most familiar constellations are the ones that are part of the zodiac. These twelve constellations can be seen in both the northern and southern hemispheres.

Patterns of Stars

• By measuring distances to stars and observing how their gravities interact with each other, scientists can determine which stars are gravitationally bound to each other. A group of stars that are gravitationally bound to each other is called a cluster.

Patterns of Stars

Star clusters

• An open cluster is a group of stars that are not densely packed.

• A globular cluster is a group of stars that are densely packed into a spherical shape.

Patterns of Stars

Star clusters

• When only two stars are gravitationally bound together and orbit a common center of mass, they are called binary stars.

• More than half of the stars in the sky are either binary stars or members of multiple-star systems.

Patterns of Stars

Binaries

• Most binary stars appear to be single stars to the human eye, even with a telescope. The two stars are usually too close together to appear separately, and one of the two is often much brighter than the other.

Patterns of Stars

Binaries

• When you look into the night sky, the stars seem to be randomly spaced from horizon to horizon. Upon closer inspection, you begin to see groups of stars that seem to cluster in one area.

Visualizing Star Groupings

Please click the image above to view the video.

• The most common way to tell that a star is one of a binary pair is to find subtle wavelength shifts, called Doppler shifts.

• Scientists use Doppler shifts to determine the speed and direction of a star’s motion.

Patterns of Stars

Doppler shifts

• When a star moves toward the observer, the light emitted by the star shifts toward the blue end of the electromagnetic spectrum. When a star moves away from the observer,its light shifts toward the red.

Patterns of Stars

Doppler shifts

• Astronomers use two units of measure for long distances. One is the light-year (ly). A light-year is the distance that light travels in one year, equal to 9.461 × 1012 km. Astronomers often use a unit larger than a light-year—a parsec (pc), which is equal to 3.26 ly, or 3.086 × 1013 km.

Stellar Positions and Distances

• When estimating the distance of stars from Earth, astronomers must account for the fact that nearby stars shift in position as observed from Earth. This apparent shift in position caused by the motion of the observer is called parallax.

Parallax

• The distance to a star can be estimated from its parallax shift by measuring the angle of the change. With advancements in technology, such as the Hipparcos satellite, astronomers can find accurate distances up to 100 pc by using the parallax technique.

Parallax

• The basic properties of a star are mass, diameter, and luminosity, which are all related to each other. Temperature is another property and is estimated by finding the spectral type of a star.

Basic Properties of Stars

• Temperature controls the nuclear reaction rate and governs the luminosity, or absolute magnitude. Apparent magnitude is how bright the stars and planets appear in the sky from Earth.

• Absolute magnitude is how bright a star would appear if it were placed at a distance of 10 pc. The absolute magnitude compared to the apparent magnitude is used to find the distance to a star.

Magnitude

• The classification of stars by absolute magnitude allows comparisons that are based on how bright the stars would appear at equal distances from an observer. The disadvantage of absolute magnitude is that it can be difficult to determine unless the actual distance to a star is known.

Magnitude

• Apparent magnitudes do not give an actual measure of energy output. To measure the energy output from the surface of a star per second, called its power or luminosity, an astronomer must know both the star’s apparent magnitude and how far away it is.

Magnitude

• Luminosity is measured in units of energy emitted per second, or watts. The Sun’s luminosity is about 3.85 × 1026 W. The values for other stars vary widely, from about 0.0001 to more than 1 million times the Sun’s luminosity. No other stellar property varies as much.

Magnitude

• Stars are assigned spectral types in the following order: O, B, A, F, G, K, and M. Each class is subdivided into more specific divisions with numbers from 0 to 9.

Classification of Stars

Temperature

• The classes were originally based only on the pattern of spectral lines, but astronomers later discovered that the classes also correspond to stellar temperatures, with the O stars being the hottest and the M stars being the coolest. Thus, by examination of a star’s spectrum, it is possible to estimate its temperature.

Temperature

• Temperature is also related to luminosity and absolute magnitude. Hotter stars put out more light than stars with lower temperatures.

• Distance can be determined by calculating a star’s luminosity based on its temperature.

Temperature

• All stars, including the Sun, have nearly identical compositions, despite differences in their spectra. The differences in the appearance of their spectra are almost entirely a result of temperature differences.

Composition

• Typically, about 73 percent of a star’s mass is hydrogen, about 25 percent is helium, and the remaining 2 percent is composed of all the other elements.

Composition

• A Hertzsprung-Russell diagram (H-R diagram) is a graph that relates stellar characteristics— class, mass, temperature, diameter, and luminosity.

• Absolute magnitude is plotted on the vertical axis and temperature or spectral type is plotted on the horizontal axis.

H-R diagrams

• Most stars occupy the region in the diagram called the main sequence, which runs diagonally from the upper-left corner, where hot, luminous stars are represented, to the lower-right corner, where cool, dim stars are represented.

H-R diagrams

• While stars are in the main sequence, they are fusing hydrogen in their cores. As stars evolve off the main sequence, they begin to fuse helium in their cores and burn hydrogen around the core edges.

Main sequence

• A star’s mass determines almost all its other properties, including its main-sequence lifetime. The more massive a star is, the higher its central temperature and the more rapidly it burns its hydrogen fuel.

Main sequence

• Red giants are large, cool, luminous stars. They are so large—more than 100 times the size of the Sun in some cases—that Earth would be swallowed up if the Sun were to become a red giant.

Main sequence

• Small, dim, hot stars are called white dwarfs. A white dwarf is about the size of Earth but has a mass about as large as the Sun’s.

Main sequence

Most stars are part of multiple-star systems.

a. true

b. false

SECTION29.2

Section Check

a. eclipsing

b. spectroscopic

c. open cluster

d. globular cluster

What type of binary star system is discovered by observing Doppler shifts?

SECTION29.2

Section Check

a. distance

b. age

c. temperature

d. magnitude

What does the number of lines on a star’s spectra indicate?

SECTION29.2

Section Check

Essential Questions

• What is the relationship between mass and a star’s evolution?

• What are the features of massive and regular star life cycles?

• How is the universe affected by the life cycles of stars?

Stellar EvolutionSECTION29.3

• The Sun and other stars follow similar life cycles, leaving the galaxy enriched with heavy elements.

Review Vocabulary

• evolution: a radical change in composition over a star’s lifetime

New Vocabulary

nebula

protostar

neutron star

pulsar

supernova

black hole

• The more massive a star is, the greater the gravity pressing inward, and the hotter and more dense the star must be inside to balance its own gravity. The temperature inside a star governs the rate of nuclear reactions, which in turn determines the star’s energy output—its luminosity.

Basic Structure of Stars

Mass effects

• The balance between gravity squeezing inward and outward pressure is maintained by heat due to nuclear reactions and compression.

• This balance, governed by themass of the star, is called hydrostatic equilibrium, and it must hold for any stable star.

Mass effects

• The density and temperature increase toward the center of a star, where energy is generated by nuclear fusion.

Fusion

• Eventually, when its nuclear fuel runs out, a star’s internal structure and mechanism for producing pressure must change to counteract gravity. The changes a star undergoes during its evolution begin with its formation.

Stellar Evolution

• The formation of a star begins with a cloud of interstellar gas and dust, called a nebula (plural, nebulae), which collapses on itself as a result of its own gravity.

• As the cloud contracts, its rotation forces it into a disk shape with a hot, condensed object at the center, called a protostar.

Stellar Evolution

Star formation

• Friction from gravity continues to increase the temperature of the protostar, until the condensed object reaches the ignition temperature for nuclear reactions and becomes a new star.

Stellar Evolution

Star formation

• The first nuclear fusion reaction to ignite in a protostar is always the conversion of hydrogen to helium. Once this reaction begins, the star becomes stable because it then has sufficient internal heat to produce the pressure needed to balance gravity. The object is then truly a star.

Stellar Evolution

Fusion begins

• It takes about 10 billion years for a star with the mass of the Sun to convert all of the hydrogen in its core into helium. Thus, such a star has a main-sequence lifetime of 10 billion years. From here, the next step in the life cycle of a small mass star is to become a red giant.

Life Cycles of Stars Like the Sun

• When the hydrogen in a star’s core is gone, it has a helium center and outer layers made of hydrogen-dominated gas. Some hydrogen continues to react in a thin layer at the outer edge of the helium core. The energy produced in this layer forces the outer layers of the star to expand and cool.

Red giant

• While a star is a red giant, it loses gas from its outer layers. Meanwhile, the core of the star becomes hot enough, at 100 million K, for helium to react and form carbon. When the helium in the core is depleted, the star is left with a core made of carbon.

SECTION29.3

Red giant

Stellar Evolution

• A star with the same mass as the Sun never becomes hot enough for carbon to fuse, so its energy production ends. The outer layers expand again and are expelled by pulsations that develop in the outer layers. The shell of gas is called a planetary nebula.

The final stages

• In the center of a planetary nebula, the core of the star becomes exposed as a small, hot object about the size of Earth. The star is then a white dwarf made of carbon.

The final stages

• A white dwarf is stable despite its lack of nuclear reactions because it is supported by the resistance of electrons being squeezed together. This pressure counteracts gravity and can support the core as long as the mass of the remaining core is less than about 1.4 times the mass of the Sun.

Internal pressure in white dwarfs

• A more massive star begins its life with hydrogen being converted to helium, but it is much higher on the main sequence. The star’s lifetime in this phase is short because the star is very luminous and uses up its fuel quickly. When the white dwarf cools and loses its luminosity, it becomes an undetectable black dwarf.

Life Cycles of Massive Stars

• A massive star undergoes many more reaction phases and thus produces a rich stew of many elements in its interior. The star becomes a red giant several times as it expands following the end of each reaction stage.

Supergiant

• As more shells are formed by the fusion of different elements in a massive star, the star expands to a larger size and becomes a supergiant. These stars are the source of heavier elements in the universe.

Supergiant

• A star that begins with a mass between about 8 and 20 times the Sun’s mass will end up with a core that is too massive to be supported by electron pressure. Once reactions in the core of the star have created iron, no further energy-producing reactions can occur, and the core of the star violently collapses in on itself.

Supernova formation

• A neutron star is a collapsed, dense core of a star that forms quickly while its outer layers are falling inward. It has a diameter of about 20 km and a mass 1.4 to 3 times that of the Sun, and it contains mostly neutrons.

Supernova formation

• A pulsar is a spinning neutron star that exhibits a pulsing pattern.

Supernova formation

• When the outer layers of a star collapse into the neutron core, the central mass of neutrons creates a pressure that causes this mass to explode outward as a supernova, leaving a neutron star.

Supernova formation

• A star that begins with more than 20 times the Sun’s mass will be too massive to form a neutron star. The resistance of neutrons to being squeezed is not great enough to stop the collapse. The core of the star continues to collapse, compacting matter into a smaller volume.

Black holes

• A black hole is a small, extremely dense remnant of a star whose gravity is so immense that not even light can escape its gravity field.

Black holes

The diagram depicts a star that is stable and will not expand or contract. What is this balance called?

a. electrostatic equilibrium

b. hydrostatic equilibrium

c. gravitational equilibrium

d. luminosity equilibrium

SECTION29.3

Section Check

The density of a neutron star is comparable to that of an atomic nucleus.

a. true

b. false

SECTION29.3

Section Check

If light cannot escape a black hole, how do astronomers locate black holes?

Answer: Because light cannot escape, a black hole is invisible. However, gases spiraling into a black hole emit X rays. Astronomers can locate the black hole by looking for those X-ray emissions.

SECTION29.3

Section Check

Resources

CHAPTER

Chapter Assessment Questions

Standardized Test Practice

Study Guide

Earth Science Online

Click on a hyperlink to view the corresponding feature.

• The Sun contains most of the mass of the solar system and has many features typical of other stars.

• Most of the mass in the solar system is found in the Sun.

• The Sun’s average density is approximately equal to that of the gas giant planets.

Study Guide

SECTION29.1

The Sun

• The Sun has a layered atmosphere.

• The Sun’s magnetic field causes sunspots and other solar activity.

• The fusion of hydrogen into helium provides the Sun’s energy and composition.

Study Guide

SECTION29.1

The Sun

• Stellar classification is based on measurement of light spectra, temperature, and composition.

• Most stars exist in clusters held together by their gravity.

• The simplest cluster is a binary.

Study Guide

SECTION29.2

Measuring the Stars

• Parallax is used to measure distances to stars.

• The brightness of stars is related to their temperature.

• Stars are classified by their spectra.

• The H-R diagram relates the basic properties of stars: class, temperature, and luminosity.

Study Guide

SECTION29.2

Measuring the Stars

• The Sun and other stars follow similar life cycles, leaving the galaxy enriched with heavy elements.

• The mass of a star determines its internal structure and its other properties.

• Gravity and pressure balance each other in a stable star.

Study Guide

SECTION29.3

Stellar Evolution

• If the temperature in the core of a star becomes high enough, elements heavier than hydrogen can fuse together.

• A supernova occurs when the outer layers of the star bounce off the neutron star core, and explode outward.

Study Guide

SECTION29.3

Stellar Evolution

The diagram shows a star with a helium core. At which stage of its life cycle is this star?

a. main sequence

b. red giant

c. white dwarf

d. helium-carbon

Chapter Assessment

CHAPTER

29 Stars

Which is the outermost layer of the Sun?

a. corona

b. prominence

c. chromosphere

d. photosphere

Chapter Assessment

CHAPTER

29 Stars

What is the difference between absolute magnitude and apparent magnitude?

Possible answer: Apparent magnitude is how bright a star appears to be from Earth. Absolute magnitude takes the star’s distance into account.

Chapter Assessment

CHAPTER

29 Stars

How is parallax used to determine the distance from Earth to a star?

Chapter Assessment

CHAPTER

29 Stars

Answer: As Earth orbits the Sun, nearby stars appear to shift position in the sky when compared with more distant stars. The closer the star, the greater the shift. By measuring the angle of the change, astronomers can estimate the distance to the star.

Chapter Assessment

CHAPTER

29 Stars

What causes the dark bands in a star’s spectrum?

Answer: The various chemical elements that make up the star absorb light at specific wavelengths. This causes dark bands to appear in the star’s spectrum.

Chapter Assessment

CHAPTER

29 Stars

a. radioactive decay

b. X-ray emissions

c. fusion reactions

d. nuclear fission

Where does the Sun’s energy come from?

CHAPTER

29 Stars

What do astronomers measure to determine a star’s motion relative to Earth’s?

a. wavelength shift

b. absolute magnitude

c. angle of parallax

d. apparent magnitude

CHAPTER

29 Stars

a. age and size

b. position

c. color and size

d. spectral type

Which do astronomers use to classify a star?

CHAPTER

29 Stars

a. protostar

b. main sequence

c. beginning stages

d. final stages

At which part of its life cycle is a Sun-sized star with a carbon core?

CHAPTER

29 Stars

a. apparent magnitude

b. absorption spectra

c. absolute magnitude

d. emission spectra

Which property takes a star’s distance into account?

CHAPTER

29 Stars

chapter 29: stars earth science geology, the environment and the universe

sunthe sunsection29

suns mass

photospherethe sunsection29

chromospherethe sunsection29

suns atmosphereoutside

suns atmospherecoronagas

suns atmospherethe photosphere

suns average density

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