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a) What is a runaway greenhouse effect? (b) What is a runaway icehouse effect?

Short Answer

Expert verified
A runaway greenhouse effect is a positive feedback loop where increasing amounts of greenhouse gases lead to higher temperatures, which in turn release more greenhouse gases. A runaway icehouse effect is when cooling leads to increased ice and snow cover, which reflects sunlight and causes further cooling.

Step by step solution

01

Define Runaway Greenhouse Effect

A runaway greenhouse effect happens when a planet's atmosphere contains gases that effectively trap heat, causing the planet's temperature to increase. This increase can then cause more of these greenhouse gases to be released, setting off a positive feedback loop that can lead to extremely high temperatures, such as those on Venus.
02

Define Runaway Icehouse Effect

A runaway icehouse effect is essentially the opposite. It occurs when a feedback effect causes a planet's temperature to decrease, leading to greater and greater amounts of ice and snow cover. As the ice and snow reflect sunlight, less heat is absorbed by the planet, causing further cooling in a self-reinforcing cycle. Earth has experienced this effect in the past during periods known as 'snowball earth' episodes.

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Key Concepts

These are the key concepts you need to understand to accurately answer the question.

Runaway Icehouse Effect
The concept of the runaway icehouse effect is synonymous with a planet's descent into an intense and prolonged period of cooling. This cooling phase evolves in a mutually reinforcing manner, where the presence of ice and snow amplifies the planet's albedo. Albedo is a measure of how much sunlight a surface reflects; ice surfaces have a high albedo, meaning they reflect a significant portion of the sun's energy back into space. As the reflective ice expands, less solar energy is absorbed by the planet, leading to even colder temperatures. This triggers a spontaneous cycle of cooling and ice expansion that may culminate in a global ice age—a condition that our planet has previously encountered in the geologic record. These periods are often referred to as 'snowball earth' events.

While the runaway icehouse effect is a natural and historical phenomenon, understanding it offers valuable insights into the intricate balance required to maintain a planet's climate within a range conducive to its prevailing life forms. It serves as a stark contrast to global warming trends, illustrating the complex nature of climate systems and the importance of feedback mechanisms that can push a planet's climate to either extreme.
Positive Feedback Loop
In the context of climate science, a positive feedback loop is a process that reinforces an initial change, potentially leading to further intensified effects. This loop works much like the sound feedback you might hear when a microphone is too close to a speaker—the noise gets louder and louder until it's overwhelmingly piercing. In planetary climates, a positive feedback loop can fuel changes that push the climate system out of balance. For instance, as temperatures rise, more water vapor (a potent greenhouse gas) may enter the atmosphere, trapping additional heat and thus raising temperatures further. This process can fuel a cascade of events, like melting ice, which reduces albedo and leads to additional warming.

The study of these feedback loops is critical, as they are powerful agents in the amplification of initial climatic changes, whether it's global warming or cooling. By understanding these loops, we can better predict and perhaps mitigate adverse effects on Earth's climate before they become self-sustaining and irreversible.
Climate Feedback Mechanisms
Climate feedback mechanisms are processes that can either amplify (positive feedback) or diminish (negative feedback) the effects of climate drivers, such as greenhouse gases. These mechanisms are the 'checks and balances' in the climate system, determining how sensitive the planet is to changes in factors like CO2 levels. For example, the melting of polar ice caps is a positive feedback mechanism; as ice melts, it exposes darker land or ocean surfaces that absorb more sunlight, which leads to additional warming and more ice melting. On the flip side, increased cloud cover can serve as a negative feedback mechanism, reflecting sunlight away and potentially cooling the Earth's surface.

The interplay of these feedbacks is a critical component of Earth's climate system that drives long-term climate stability or change. They are integral to various climate models and are essential for scientists to make accurate predictions. Learning about these mechanisms equips us with the knowledge required for informed decision-making regarding environmental policies and climate change mitigation strategies.

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Most popular questions from this chapter

The classic 1950 science-fiction movie Rocketship X-M shows astronauts on the Martian surface with oxygen masks for breathing but wearing ordinary clothing. Would this be a sensible choice of apparel for a walk on Mars? Why or why not?

Use the Starry Night Enthusiast \({ }^{\mathrm{TM}}\) program to observe the appearance of Mars. Select Favourites \(>\) Guides \(>\) Atlas from the menu. Select View \(>\) Celestial Grid from the menu to turn this option off. Open the Find pane and click the menu button for Mars and choose Centre from the menu. Close the Find pane and then use the Zoom controls in the toolbar to set a field of view of approximately \(58^{\prime \prime} \times 40^{\prime \prime}\). (a) Set the Time Flow Rate to 1 hour and then run Time Forward. Describe what you see. (b) Stop time flow. Change the Time Flow Rate to 1 lunar month. Run Time Forward again. Describe what you see. Using a diagram like Figure 4-6, explain the changes in the apparent size of the planet. (c) Stop time flow and zoom out to a field of view of approximately \(\mathbf{2}^{\prime} \times \mathbf{1}^{\prime}\). Change the time and date in the toolbar to \(12: 00: 00\) A.M. on August 28, 2003, to see Mars during a very favourable opposition. You will see Mars and its two moons, Phobos and Deimos. In the toolbar, set the Time Flow Rate to 1 minute. Record the date and time in the display, and note the position of Phobos (the inner moon). Click the Run Time Forward and single time step button (the rightmost time control button) to advance time until Phobos returns to approximately the same position relative to Mars. Record the date and time in the display. From your observations, what is the orbital period of Phobos? How does your result compare with the orbital period given in Appendix 3? (d) Repeat part (c) for Deimos (the outer moon).

Refer to the Universe Web site or eBook for a link to a Web site that calculates the dates of upcoming greatest elongations of Mercury. Consult such magazines as Sky or Telescope and Astronomy, or the Web sites for these magazines, to determine if any of these greatest elongations is going to be a favorable one. If so, make plans to be one of those rare individuals who has actually seen the innermost planet of the solar system. Set aside several evenings (or mornings) around the date of the favorable elongation to reduce the chances of being "clouded out." Select an observing site that has a clear, unobstructed view of the horizon where the Sun sets (or rises). If possible, make arrangements to have a telescope at your disposal. Search for the planet on the dates you have selected, and make a drawing of its appearance through your telescope.

What kind of surface features are found on Mercury? How do they compare to surface features on the Moon? Why are they probably much older than most surface features on the Earth?

Why are naked-eye observations of Mercury best made at dusk or dawn, while telescopic observations are best made during the day?

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