TEKS: Chapter 112. Science See All Teacher Resources

112.36.c.5

Earth in space and time. The student understands the solar nebular accretionary disk model. The student is expected to:

• (A)  analyze how gravitational condensation of solar nebular gas and dust can lead to the accretion of planetesimals and protoplanets;

• (B)  investigate thermal energy sources, including kinetic heat of impact accretion, gravitational compression, and radioactive decay, which are thought to allow protoplanet differentiation into layers;

• (C)  contrast the characteristics of comets, asteroids, and meteoroids and their positions in the solar system, including the orbital regions of the terrestrial planets, the asteroid belt, gas giants, Kuiper Belt, and Oort Cloud;

• (D)  explore the historical and current hypotheses for the origin of the Moon, including the collision of Earth with a Mars-sized planetesimal;

• (E)  compare terrestrial planets to gas-giant planets in the solar system, including structure, composition, size, density, orbit, surface features, tectonic activity, temperature, and suitability for life; and

• (F)  compare extra-solar planets with planets in our solar system and describe how such planets are detected.