2. Why is Earth more suitable for life than Venus?
3. Are volcanoes present throughout the terrestrial planets? Why or why not?
4. How would a journey of exploration through the inner planets of our solar system differ
   from an exploration of the outer planets? Focus your response on explaining the basic
   physical characteristics of the inner and outer planets. How do the origins of our solar
   system explain these physical differences between planets?
5. Identify similarities in the origins of the following solar system objects: planetary rings,
   satellites, asteroids, comets, the Oort Cloud, and the Kuiper Belt. How do these objects’
   origins relate to the origin and formation of planets?

2. Why is Earth more suitable for life than Venus?

• Temperature: Earth has a moderate temperature range that allows for liquid water to exist, which is essential for life. Venus, on the other hand, has a thick atmosphere that traps heat, leading to surface temperatures around 467°C (872°F), which is too hot for known life forms.
• Atmosphere: Earth’s atmosphere is composed of 78% nitrogen and 21% oxygen, which supports life. Venus has a dense atmosphere primarily made up of carbon dioxide (about 96.5%) with clouds of sulfuric acid, making it inhospitable.
• Water: Earth has abundant liquid water on its surface, which is crucial for all known forms of life. Venus has very little water, and any that may have existed has likely evaporated due to the high temperatures.
• Magnetic Field: Earth has a strong magnetic field that protects it from solar and cosmic radiation. Venus has a weak magnetic field, which may expose its surface to harmful radiation.

3. Are volcanoes present throughout the terrestrial planets? Why or why not?

• Geological Activity: Planets like Earth and Mars have shown evidence of volcanic activity. Earth is geologically active with many volcanoes, while Mars has the largest volcano in the solar system, Olympus Mons, indicating past volcanic activity.
• Planetary Size and Heat: Larger planets tend to retain heat longer, which can sustain geological activity. Mercury, being smaller and having cooled significantly, shows little evidence of volcanic activity.
• Tectonic Activity: The presence of tectonic plates, as seen on Earth, can lead to volcanic activity. Mars has some tectonic features, but they are not as active as Earth’s.
• Atmospheric Conditions: The atmosphere can influence volcanic activity. For example, Venus has many volcanoes, but its thick atmosphere and high pressure create different volcanic processes compared to Earth.

4. How would a journey of exploration through the inner planets of our solar system differ from an exploration of the outer planets?

• Physical Characteristics:
  • Inner Planets: These are rocky, terrestrial planets with solid surfaces. They have a higher density and are closer to the Sun, resulting in higher temperatures and varied atmospheres.
  • Outer Planets: These are gas giants (Jupiter and Saturn) and ice giants (Uranus and Neptune) with no solid surface. They are much larger, have lower densities, and are composed mainly of hydrogen, helium, and other gases.
• Exploration Challenges:
  • Inner Planets: Missions to inner planets require technology to withstand high temperatures and radiation (especially for Venus). Landing on these planets involves dealing with solid surfaces and potential geological activity.
  • Outer Planets: Missions to outer planets face challenges such as extreme cold, high radiation levels, and the need for long-duration space travel. Exploration often involves orbiters and flybys rather than landers due to the lack of solid surfaces.
• Origins of the Solar System: The inner planets formed from the solar nebula’s rocky materials, while the outer planets formed from gas and ice in the colder regions of the solar system. This difference in formation explains their distinct physical characteristics.

5. Identify similarities in the origins of the following solar system objects: planetary rings, satellites, asteroids, comets, the Oort Cloud, and the Kuiper Belt.

• Formation from the Solar Nebula: All these objects originated from the solar nebula, the cloud of gas and dust that surrounded the young Sun. As the solar system formed, materials coalesced to create planets, moons, and other bodies.
• Gravitational Interactions: Many of these objects were shaped by gravitational interactions. For example, planetary rings can form from debris captured by a planet’s gravity, while satellites often form from the same material that created their parent planet.
• Leftover Building Blocks: Asteroids and comets are considered leftover building blocks from the early solar system. They did not coalesce into planets and remain as remnants of the solar system’s formation.
• Location and Composition: The Kuiper Belt and Oort Cloud are regions filled with icy bodies and debris, representing the outer limits of the solar system. They contain materials that did not form into planets, similar to asteroids in the asteroid belt.