Essential Science for Teachers: Earth and Space Science
Order out of Chaos: Our Solar System Order Out of Chaos: Our Solar System | A Closer Look
A Closer Look
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A Closer Look: Star Formation
The core then begins to collapse under its own weight, making it hotter and denser, and, as it gets smaller, it rotates faster in the same way that figure skaters spin faster when they pull their arms closer to their bodies. Once it begins to spin fast enough, the rotation of the gas and dust can keep material from moving toward the axis of rotation (the imaginary line about which all of the material is orbiting), but gravity keeps material falling along the axis of rotation. At this point, there is a flattened disk of material orbiting around a proto-star at the center of the disk. Some of the disk’s gas and dust will eventually fall onto the star, some will become the planets, moons, asteroids, and other objects that orbit the star, and some will escape the newly forming solar system. Eventually the solar system will settle into a state in which planets, asteroids, comets, and other bodies have stable orbits around the star, and the gas and dust have disappeared. This is the state of our solar system now.
It is possible for the core to fragment as it collapses, and the result is that more than one star is formed. In such cases, a disk of material can form around each star, around a multiple system of stars, or both. The formation of planets in such cases is not as well understood as planet formation is around an isolated star. Furthermore, it is important to remember that stars do not last forever. Eventually all stars run out of the fuel that allows them to shine, and they cool off and become less luminous, which has a significant impact on the planets orbiting the star. Fortunately for Earth, the Sun is expected to last for several billion more years before this is expected to happen.
A Closer Look: Extrasolar Planets
One way to find a planet orbiting a distant star is to continually monitor the amount of light coming from the star. If a planet’s orbit brings it between the Earth and the star, the planet will block some of the light and, from Earth, it will look like the star becomes briefly dimmer. By determining how often this happens, the period of the planet’s orbit and its distance from the star can be determined. By measuring how much light the planet blocks, it is possible to determine its size, because a larger planet will block more light.
One problem with this method of detecting planets is that only large planets that orbit very close to their host star will block enough light for astronomers to be able to measure the fluctuations in the brightness of the star. As a result, the planets found with this or any other method developed thus far are all very large (about the size of Jupiter), and many of them orbit closer to their stars than the Earth is to the Sun. Since in our solar system the largest planets all orbit the Sun much farther out than the Earth, it is a challenge to understand why these systems are so different from our own. With the next generation of telescopes and satellites, astronomers hope to be able to detect Earth-like planets at Earth-like distances from their stars. At that time, scientists will be able to determine how common or rare it is for such massive planets to be able to form so close to their stars.
A Closer Look: Meteorites
There are two kinds of places on Earth where meteorites are more likely to be found. One is on parts of the Antarctic ice cap where the ice flows together and evaporates in the sun and wind, leaving behind meteorites as a lag deposit. The other prime meteorite hunting ground is in deserts, where the dry conditions tend to preserve stones and the lack of rain means they are less likely to wash away.
Almost all meteorites come from the asteroid belt between Mars and Jupiter, where thousands of small, solid objects orbit the Sun. Some meteorites show geochemical signs of having been part of an evolving planet. Some are similar to basaltic rocks found on Earth. These basaltic meteorites are created by the impacts of other meteorites onto other bodies in the solar system, most commonly Mars and the Moon.
Session 1 Earth’s Solid Membrane: Soil
How does soil appear on a newly born, barren volcanic island? In this session, participants explore how soil is formed, its role in certain Earth processes, its composition and structure, and its place in the structure of the Earth.
Session 2 Every Rock Tells A Story
How can we use rocks to understand events in the Earth's past? In this session, participants explore the processes that form sedimentary rocks, learn how fossils are preserved, and are introduced to the theory of plate tectonics.
Session 3 Journey to the Earth’s Interior
How do we know what the interior of the Earth is like if we've never been there? In this session, participants examine the internal structure of the Earth and learn how it is possible for entire continents to move across its surface.
Session 4 The Engine That Drives the Earth
What drives the movement of tectonic plates? In this session, participants learn how plates interact at plate margins, how volcanoes work, and the story of Hawaii's formation.
Session 5 When Continents Collide
How is it possible that marine fossils are found on Mount Everest, the world's highest continental mountain? In this session, participants learn what happens when continents collide and how this process shapes the surface of the Earth.
Session 6 Restless Landscapes
If almost all mountains are formed the same way, why do they look so different? In this session, participants learn about the forces continually at work on the surface of the Earth that sculpt the ever-changing landscape.
Session 7 Our Nearest Neighbor: The Moon
Why is the Moon, our nearest neighbor in the solar system, so different from the Earth? In this session, participants explore the complex connections between the Earth and Moon, the origin of the Moon, and the roles played by gravity and collisions in the Earth-Moon system.
Session 8 Order out of Chaos: Our Solar System
Why do all the planets orbit the Sun in the same direction and why are the planets closest to the Sun so different from the gas giants farther out? In this session, participants gain a better understanding of the nature of the solar system by examining its formation.