This book is an appealing, concise, and factual account of the chemistry of the solar system. It includes basic facts about the chemical composition of the different bodies in the solar system, the major chemical processes involved in the formation of the Sun, planets and small objects, and the chemical processes that determine their current chemical make-up. There are numerous informative summary tables and data is presented in graphical form which is useful for identifying common features of the major processes that determine the current chemical state of the planets. The book will interest general readers with a background in chemistry who will enjoy reading about the chemical diversity of the solar system's objects as well as an introductory textbook for graduate classes in planetary sciences.
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Katharina Lodders is Research Professor in the Department of Earth & Planetary Sciences at Washington University in St. Louis, MO, USA. She is senior author with Dr. Fegley of The Planetary Scientist's Companion (Oxford University Press, 1998) and the author (or co-author) of over 80 refereed publications in scientific journals and books. Her experimental and theoretical research focuses on topics in cosmochemistry, planetary science, and astronomy. Bruce Fegley, Jr., is Professor of Planetary Sciences in the Department of Earth & Planetary Sciences at Washington University in St. Louis, MO, USA. He is junior author with Dr. Lodders of The Planetary Scientist's Companion (Oxford University Press, 1998) and is senior author of Practical Chemical Thermodynamics for Geoscientists (Academic-Elsevier, scheduled for 2008) with Ms. Rose Osborne. He is the author (or co-author) of over 120 refereed publications in scientific journals and books. At present and over the past 16 years he has taught several advanced undergraduate and graduate level courses in geochemistry and planetary science including "Thermodynamics and Phase Equilibria," "Planetary Geochemistry," and "Earth System Science." Dr.Fegley received his S.B. in Chemistry and PhD. in Geochemistry at MIT and has 25 years of experience in geochemistry, cosmochemistry and planetary science.
This book is an appealing, concise, and factual account of the chemistry of the solar system. The authors have set the scene by including entertaining historical accounts on how ideas developed, and together with new discoveries, shaped our current understandings. Engaging with a broad readership, the text includes basic facts about the chemical composition of the different bodies in the solar system, the major chemical processes involved in the formation of the Sun, planets, and small objects, and the chemical processes that determine their current chemical make-up. The book summarizes compositional data but focuses on the chemical processes and where relevant, it also emphasizes comparative planetology. There are numerous informative summary tables which illustrate the similarities (or differences) that help the reader to understand the processes described. Data are presented in graphical form which is useful for identifying common features of the major processes that determine the current chemical state of the planets. The book will interest general readers with a background in chemistry who will enjoy reading about the chemical diversity of the solar system's objects. It will serve as an introductory textbook for graduate classes in planetary sciences but will also be very popular with professional researchers in academia and government, college professors, and postgraduate fellows.
Some Milestones up to the Beginning of the Space Age,
Chapter 1 The Elements in the Solar System,
Chapter 2 Meteorites,
Chapter 3 The Solar Nebula,
Chapter 4 The Bodies in the Inner Solar System,
Chapter 5 Terrestrial Atmospheric Chemistry 5.1 Introduction,
Chapter 6 The Greenhouse Effect and Biogeochemical Cycles on Earth,
Chapter 7 The Outer Solar System 7.1 Introduction,
Appendix A Table of Abundances of Nuclides in the Solar System,
Appendix B Table of Average Element Concentrations in Major Chondritic Meteorite Groups,
Appendix C Review of Chemical Kinetics,
Subject Index,
The Elements in the Solar System
"Of course I was not there when the solar system originated and I do not know how it originated. I am only a student of the subject and I modify my ideas as new evidence appears or as new ideas occur to me."
Harold Urey, 1963
A founding father of cosmochemistry
1.1 INTRODUCTION
Modern evidence leads to the insight that stars and their planetary systems form by gravitational collapse of interstellar molecular clouds. Much of the chemistry in our solar system is governed by the original element inventory that the solar system inherited from its presolar molecular cloud about 4.6 billion years ago.
Molecular clouds are cosmic recycling bins for the elements produced in many stars from different generations. The big-bang endowed the universe with H, D, He (both isotopes 3He and 4He) and a dash of Li (mainly 7Li). Hydrogen and He serve as major nuclear fuel in stars. The light elements Li, Be and B have particular histories of their own (see below) but all other elements came into being through stellar nucleosynthesis over time.
Stars like our Sun and ones that are more massive do not exist forever. In its final evolutionary stage, a star returns most of its mass – including mass in the form of freshly synthesized elements – back to the interstellar medium. The efficiency and yields for element production depends on the initial mass of the star, which also determines whether the newly produced elements are released through a stellar explosion as a supernova, or by less violent stellar winds. The result is that the stellar "ashes" can become part of the molecular clouds in the interstellar medium from which new generations of stars can rise.
Element production in generations of stars has been ongoing since the time the universe formed some 14 billion years ago. It is still ongoing in the stars that we can see in our galaxy and in stars of other galaxies dispersed in the universe. There is no need to worry that stars will disappear soon because there is no H and He left as initial stellar fuel. On a universal scale, H and He remain the most abundant elements. At the Sun's birthplace in our galaxy, the mass fraction of all elements heavier than helium had increased only to about 1.5% between the time when element production in stars of our Milky Way Galaxy started and the solar system formed. The rather low abundance of all heavy elements compared to H and He is one reason why astronomers collectively call all elements heavier than helium "metals." This definition of "metals" is not the traditional characterization that one normally associates with metals. On the other hand, there is the natural bias from daily life on a planet that essentially only consists of these "metals."
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