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Solutions Manual — Earth: Portrait of a Planet, 5th Edition — Stephen Marshak — ISBN 9780393937503 — Latest Update 2025/2026 — (All Chapters Covered 1–25)

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This comprehensive Solutions Manual for Earth: Portrait of a Planet (5th Edition) by Stephen Marshak delivers detailed, step-by-step answers for all core topics in planetary science, geology, Earth systems, and environmental processes. Ideal for both instructors and students, this resource supports conceptual learning, quantitative reasoning, and application-based problem solving across every instructional unit, strictly aligned to the official chapter sequence. The chapter flow begins with Chapter 1: The Universe and the Earth, which introduces cosmology and the formation of Earth within the universe, followed by Chapter 2: Journey to the Center of the Earth, which explains Earth's internal structure and geophysical investigation methods. Chapter 3: Plate Tectonics explores the dynamic behavior and boundaries of tectonic plates, and Chapter 4: The Way the Earth Works: Plate Tectonics outlines how these forces shape the planet’s surface over geologic time. In Chapter 5: The Earth Materials, the focus shifts to minerals—their formation, properties, and classification—while Chapter 6: Igneous Rocks details the rock cycle and characteristics of magmatic formations. Chapter 7: Sedimentary Rocks examines the processes of weathering, erosion, and sedimentation, and Chapter 8: Metamorphism explores the transformation of rocks under pressure and temperature changes. The manual continues with Chapter 9: Volcanic Activity, analyzing eruption types and associated hazards, and Chapter 10: Earthquakes, which investigates seismic events and crustal deformation. Chapter 11: Mountain Building discusses orogenic processes and structural geology. Chapter 12: Deep Time reconstructs Earth's prehistorical past using stratigraphy and radiometric dating, while Chapter 13: Evolutionary History of Life examines the fossil record and mass extinctions throughout geologic time. In Chapter 14: Energy Resources, students explore fossil fuels, geothermal energy, and extraction technologies, followed by Chapter 15: Mineral Resources, which highlights ore formation, mining, and environmental impacts. Chapter 16: Mass Wasting covers slope stability, landslides, and related hazards. Chapter 17: Streams and Floods introduces fluvial processes and floodplain dynamics, while Chapter 18: Groundwater explains aquifer behavior and water resource sustainability. Chapter 19: Deserts, Chapter 20: Coastal Landscapes, and Chapter 21: The Atmosphere collectively address Earth's surface interactions, weathering, wave action, and atmospheric behavior. The manual concludes with Chapter 22: Weather Systems and Climate, which examines global weather patterns, Chapter 23: Glacial Landscapes, exploring the effects of ice on topography, Chapter 24: Global Climate Change, discussing long-term shifts, human influence, and feedback mechanisms, and Chapter 25: Earth Systems Science, which synthesizes knowledge of Earth as a complex, interactive system impacted by both natural forces and human activity.

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Earth: Portrait of a Planet
5th Edition
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SOLUTIONS
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MANUAL
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Stephen Marshak
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Comprehensive Solutions Manual for
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Instructors and Students
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© Stephen Marshak. All rights reserved. Reproduction or distribution without permission is

prohibited.




©MedConnoisseur

, Solutions Manual for Earth Portrait of a
Planet, 5e, by Stephen Marshak (All Chapters)

CHAPTER 1
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Cosmology and the Birth of Earth
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Learning Objectives

1. Students should be aware of the Big Bang theory and the major evidence
supporting it. Distant galaxies are uniformly red-shifted rather than blue-
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shifted; this implies that they are all moving away from us. The farthest
galaxies are those that are most strongly red-shifted, meaning that they are
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receding the fastest. Extrapolation of velocities and trajectories into the past
suggests that all matter in the Universe was contained in a single point,
approximately 13.7 billion years ago. At that time, the Universe explosively
came into existence.
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2. Stars, including our Sun, are nuclear fusion reactors. For most of their life
histories (on the order of billions of years), hydrogen atoms are fused together
to form helium. Later stages in stellar evolution include fusion of helium atoms
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and other, heavier elements; ultimately, iron is the heaviest element that can
be produced through fusion reactions within stars.
3. After their cycles of fusion are complete, large stars violently explode (forming
supernovae), producing elements heavier than iron and leaving behind a
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residue of diffuse nebulae, which may be recycled to form a new star at some
point in the future.
4. Our Solar System is approximately 4.57 Ga (billion years old). All eight planets
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revolve around the Sun in coplanar, elliptical orbits. All planets orbit in the




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, same direction (counterclockwise as viewed from above Earth’s North Pole).
These facts imply simultaneous planetary formation from a swirling nebula
surrounding the Sun (the similarities in orbits would then be a natural result of
conservation of angular momentum). The planets accreted from this nebula
through gravitational attraction and haphazard collisions. Pluto, long
considered the “ninth planet,” has seen its status demoted; astronomers now
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recognize eight major planets.
5. The terrestrial planets (Mercury, Venus, Earth, and Mars) are relatively small,
dense, and rocky worlds. The giant planets are predominantly composed of the
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light gases hydrogen and helium (Jupiter and Saturn) or ices (Uranus and
Neptune); they are much larger and much less dense than the terrestrial
planets.
6. Our Moon is chemically similar to the Earth’s mantle. The Moon is thought to
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have originated from debris accumulated when a protoplanet collided with
Earth approximately 4.3 Ga.
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Summary from the Text

The geocentric model placed Earth at the center of the Universe, with the planets
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and Sun orbiting around the Earth within a celestial sphere speckled with stars. The
heliocentric model, which gained acceptance during the Renaissance, placed the Sun
at the center.
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Eratosthenes was able to measure the size of Earth in ancient times, but it was
not until fairly recently that astronomers accurately determined the distances to the
Sun, planets, and stars. Distances in the Universe are so large that they must be
measured in light-years.
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The Earth is one of eight planets orbiting the Sun, and this Solar System lies on
the outer edge of a slowly revolving galaxy, the Milky Way, which is composed of
about 300 billion stars. The Universe contains at least hundreds of billions of galaxies.
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The red shift of light from distant galaxies, a manifestation of the Doppler effect,
indicates that all distant galaxies are moving away from Earth. This observation leads




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, to the expanding Universe theory. Most astronomers agree that this expansion began
after the Big Bang, a cataclysmic explosion about 13.7 billion years ago.
The first atoms (hydrogen and helium) of the Universe developed within minutes
of the Big Bang. These atoms formed vast gas clouds, called nebulae.
Gravity caused clumps of gas in the nebulae to coalesce into revolving balls. As
these balls of gas collapsed inward, they evolved into flattened disks with bulbous
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centers. The protostars at the center of these disks eventually became dense and
sufficiently hot that fusion reactions began within them. When this happened, they
became true stars, emitting heat and light.
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Heavier elements form during fusion reactions in stars; the heaviest are mostly
made during supernova explosions. Earth and the life forms on it contain elements
that could have only been produced during the life cycle of stars. Thus, we are all
made of stardust.
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According to the nebular theory of planet formation, planets developed from the
rings of gas and dust surrounding protostars. The gas and dust condensed into
planetesimals, which then clumped together to form protoplanets and finally true
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planets. Inner rings became the terrestrial planets; outer rings grew into giant
planets.
The Moon formed from debris ejected when a protoplanet collided with Earth in
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the young Solar System.
A planet assumes a near-spherical shape when it becomes so soft that gravity can
smooth out irregularities.
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Answers to Review Questions

1. Why do the planets appear to move with respect to the stars?
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ANS: Stars are so relatively distant that they appear fixed with respect to one
another as viewed from Earth. As Earth and the other planets traverse through their
orbits around the Sun, the positions of the planets vary with respect to the “fixed”
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celestial sphere.




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