文档介绍：Understanding Earth
Fifth Edition
Chapter 9:
EARLY HISTORY OF THE TERRESTRIAL S
Copyright © 2007 by W. H. Freeman pany
Grotzinger • Jordan • Press • Siever
Chapter 9
Early History of the Terrestrial s
(地球的初期歷史)
About Terrestrial s(類地行星)
The solar system and its s formed
around the Sun.
(太陽系與太陽系的行星圍繞著太陽而形成)
The s differentiated into layered
bodies.
(行星分異成層狀體)
The geologic processes that formed
Mercury, Venus, Earth, Moon, and Mars
are similar in many ways.
(形成水星、金星、地球、月亮與火星的地質作
用有許多相似之處)
Lecture Outline
Origin of the solar system (太陽系的起源)
2. Early Earth: forming a layered
(初始的地球:形成一個層狀的行星)
3. Diversity of the s (行星間的差異)
4. Age plexion of ary
surfaces (行星的年齡與表面的特徵)
5. Mars rocks! (火星的岩石)
6. Exploring the solar system and beyond
(探勘太陽系與更遙遠的太空)
Origin of the solar system
(太陽系的起源)
● The nebular hypothesis
(星雲假說)
● the sun forms (太陽形成)
● the s form (行星形成)
● esimals (小行星體)
● inner s (內行星群)
● outer s (外行星群)
1. Origin of the solar system
The nebular hypothesis
Bya, the Big Bang occurs
Gas cloud begins to contract under the force of gravity
Contraction causes cloud to speed up ( think Ice skaters)
Faster rotation causes cloud to flatten into a disk
The sun forms
Proto-Sun, where most of the nebula material is located
The s form
Particles begin to condense as the disk cools
esimals form from the collision of these particles
Inner s - small, rocky s, too close to the Sun for volatiles to exist in great quantity
Outer s - composed ice and gases formed from volatiles that were sent to the reaches of the solar system
約在一千萬年內由小型星聚合為內行星,且較輕的氣體如氫、氦、水蒸氣被太陽風吹走
、
行星體積與質量較大,可吸引住較輕的氣體如氫、氦。具石質或鐵質內核