The study of presolar meteoritic grains is a new inter-disciplinary field that brings together topics from nuclear physics to astronomy and chemistry. Traditionally, most of the information about the cosmos has been gathered by observing light through telescopes. However, with the recent discovery that some dust grains extracted from primitive meteorites were produced in stellar environments, we now have the opportunity to gather information about stars and our Galaxy from the laboratory analysis of tiny pieces of stardust. Stellar grains represent a unique and fascinating subject of study. Their analysis is a breakthrough in research on stellar nucleosynthesis and the origin of the elements. While a number of specialized reviews exist on the topic, this book is the first work that brings together in a unified and accessible manner the background knowledge necessary for the study of presolar grains together with up-to-date discoveries in the field. The book includes exercise questions and answers, an extensive glossary for easy reference, and more than 40 figures and tables -- from schematic diagrams to electron microscope images and graphs of results from stellar grain measurements and theoretical stellar models

lgli/dvd69/Lugaro M. Stardust from Meteorites[c] An Introduction to Presolar Grains (2005)(en)(209s).pdf

lgrsnf/dvd69/Lugaro M. Stardust from Meteorites[c] An Introduction to Presolar Grains (2005)(en)(209s).pdf

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zlib/Physics/Astronomy: Astrophysics/Maria Lugaro/Stardust from Meteorites: An Introduction to Presolar Grains (2005)(en)(209s)_502191.pdf

Lugaro, Maria

World Scientific Publishing Co Pte Ltd

World Scientific series in astronomy and astrophysics, v. 9, New Jersey ; London, 2005

World Scientific series in astronomy and astrophysics, v. 9, Singapore, ©2005

World Scientific Publishing Company, Singapore, 2005

Singapore, Singapore

September 2005

mexmat -- 69

lg70325

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Contents......Page 12
Preface......Page 8
1 . Meteoritic Presolar Grains and Their Significance......Page 16
1.1 Presolar isotopic signatures and their carriers......Page 18
1.2 The discovery of presolar stellar grains......Page 23
1.3 Meteorites carrying stellar grains......Page 25
1.4 Types of presolar grains......Page 26
1.4.1 Diamonds......Page 28
1.4.3 Silicon carbide grains......Page 29
1.4.4 Graphite grains......Page 31
1.4.6 Silicon nitride grains......Page 32
1.5.1 Stellar evolution, nucleosynthesis and mixing......Page 33
1.5.2 Physical and chemical properties of the gas around stars and supernov......Page 35
1.5.3 The interstellar medium, molecular clouds and early solar system......Page 37
1.7 Exercises......Page 39
2 . Basics of Stellar Nucleosynthesis......Page 40
2.1 Hydrogen burning, and the life of most stars......Page 42
2.1.1 The pp chain......Page 44
2.1.2 The CNO, NeNa and MgAl cycles......Page 47
2.2 Helium burning, and the evolution of stars of low mass......Page 51
2.3 The process: C, Ne and O burnings, and the evolution of stars of high mass......Page 54
2.4 The e process: Si burning, and supernova explosions......Page 55
2.5 The production of elements heavier than Fe......Page 60
2.5.1 The s process......Page 64
2.5.2 The r process......Page 66
2.5.3 The p process......Page 71
2.6 Exercises......Page 72
3.1 The isolation of diamond, graphite and SiC grains......Page 74
3.2 Looking at presolar grains......Page 77
3.3 Isotopic measurements with mass spectrometers......Page 78
3.3.2 Secondary Ion Mass Spectrometry (SIMS)......Page 80
3.3.3 The advent of Resonant Ionization Mass Spectrometry (RIMS) in trace element analysis......Page 83
3.4 Location and analysis of rare types of presolar grains......Page 86
3.5 Concluding remarks......Page 89
3.6 Exercises......Page 90
4.1 Classification of Sic grains on the basis of their C, N and Si compositions......Page 92
4.2 Where did mainstream presolar Sic grains come from?......Page 96
4.2.1 Theoretical modelling of AGB and C(N) stars......Page 98
4.3 Carbon and nitrogen in mainstream Sic grains and in AGB stars......Page 103
4.4 The Ne-E(H) anomalous component......Page 109
4.5 The presence of 26Al......Page 113
4.6 The puzzle of the silicon isotopic composition of mainstream Sic grains......Page 114
4.7 Titanium isotopic composition of mainstream Sic grains......Page 120
4.8.1 The Y and Z populations......Page 123
4.8.2 The A and B populations......Page 124
4.8.3 The X population......Page 125
4.9 Exercises......Page 126
5 . Heavy Elements in Presolar SiC Grains......Page 128
5.1 Modelling the s process in AGB stars......Page 129
5.1.1 The neutron source in AGB stars......Page 130
5.1.2 The production of a 13C pocket......Page 132
5.1.3 The current model......Page 136
5.1.4 The neutron flux in the 13C pocket......Page 138
5.1.5 The neutron flux in the thermal pulse......Page 139
5.2.1 Class I: Isotopic ratios involving p-only and r-only isotopes......Page 141
5.2.2 Class II: Isotopic ratios involving isotopes in local equilibriuin......Page 145
5.2.3 Class III: Isotopic ratios involving isotopes with magic neutron numbers......Page 147
5.2.4 Class IV: Isotopic ratios involving isotopes depending on branchings......Page 152
5.2.5 Class V: Isotopic ratios involving isotopes produced by radioactive decay......Page 156
5.3 The heavy noble gases: Kr and Xe......Page 157
5.4 Exercises......Page 162
6.1 Diamond......Page 166
6.2 Graphite......Page 169
6.3 Oxide grains......Page 172
6.4 Exercises......Page 177
Appendix A Glossary......Page 180
B.2 Chapter 2......Page 188
B.3 Chapter 3......Page 190
B.4 Chapter 4......Page 192
B.5 Chapter 5......Page 194
B.6 Chapter 6......Page 196
C.2 Stellar evolution and nucleosynthesis......Page 198
C.3 AGB stellar evolution and nucleosynthesis......Page 199
Bibliography......Page 200
Index......Page 222

Contents 12
Preface 8
1 . Meteoritic Presolar Grains and Their Significance 16
1.1 Presolar isotopic signatures and their carriers 18
1.2 The discovery of presolar stellar grains 23
1.3 Meteorites carrying stellar grains 25
1.4 Types of presolar grains 26
1.4.1 Diamonds 28
1.4.2 Silicate grains 29
1.4.3 Silicon carbide grains 29
1.4.4 Graphite grains 31
1.4.5 Oxide grains 32
1.4.6 Silicon nitride grains 32
1.5 New information from presolar grains 33
1.5.1 Stellar evolution, nucleosynthesis and mixing 33
1.5.2 Physical and chemical properties of the gas around stars and supernov 35
1.5.3 The interstellar medium, molecular clouds and early solar system 37
1.6 Outline 39
1.7 Exercises 39
2 . Basics of Stellar Nucleosynthesis 40
2.1 Hydrogen burning, and the life of most stars 42
2.1.1 The pp chain 44
2.1.2 The CNO, NeNa and MgAl cycles 47
2.2 Helium burning, and the evolution of stars of low mass 51
2.3 The process: C, Ne and O burnings, and the evolution of stars of high mass 54
2.4 The e process: Si burning, and supernova explosions 55
2.5 The production of elements heavier than Fe 60
2.5.1 The s process 64
2.5.2 The r process 66
2.5.3 The p process 71
2.6 Exercises 72
3 . Laboratory Analysis of Presolar Grains 74
3.1 The isolation of diamond, graphite and SiC grains 74
3.2 Looking at presolar grains 77
3.3 Isotopic measurements with mass spectrometers 78
3.3.1 Noble-gas extraction 80
3.3.2 Secondary Ion Mass Spectrometry (SIMS) 80
3.3.3 The advent of Resonant Ionization Mass Spectrometry (RIMS) in trace element analysis 83
3.4 Location and analysis of rare types of presolar grains 86
3.5 Concluding remarks 89
3.6 Exercises 90
4 . The Origin of Presolar Sic Grains 92
4.1 Classification of Sic grains on the basis of their C, N and Si compositions 92
4.2 Where did mainstream presolar Sic grains come from? 96
4.2.1 Theoretical modelling of AGB and C(N) stars 98
4.3 Carbon and nitrogen in mainstream Sic grains and in AGB stars 103
4.4 The Ne-E(H) anomalous component 109
4.5 The presence of 26Al 113
4.6 The puzzle of the silicon isotopic composition of mainstream Sic grains 114
4.7 Titanium isotopic composition of mainstream Sic grains 120
4.8 A, B, X, Y and Z: The minor Sic grains populations 123
4.8.1 The Y and Z populations 123
4.8.2 The A and B populations 124
4.8.3 The X population 125
4.9 Exercises 126
5 . Heavy Elements in Presolar SiC Grains 128
5.1 Modelling the s process in AGB stars 129
5.1.1 The neutron source in AGB stars 130
5.1.2 The production of a 13C pocket 132
5.1.3 The current model 136
5.1.4 The neutron flux in the 13C pocket 138
5.1.5 The neutron flux in the thermal pulse 139
5.2 SiC grain data and the s process in AGB stars 141
5.2.1 Class I: Isotopic ratios involving p-only and r-only isotopes 141
5.2.2 Class II: Isotopic ratios involving isotopes in local equilibriuin 145
5.2.3 Class III: Isotopic ratios involving isotopes with magic neutron numbers 147
5.2.4 Class IV: Isotopic ratios involving isotopes depending on branchings 152
5.2.5 Class V: Isotopic ratios involving isotopes produced by radioactive decay 156
5.3 The heavy noble gases: Kr and Xe 157
5.4 Exercises 162
6 . Diamond, Graphite and Oxide Grains 166
6.1 Diamond 166
6.2 Graphite 169
6.3 Oxide grains 172
6.4 Exercises 177
Appendix A Glossary 180
Appendix B Solutions to Exercises 188
B.l Chapter 1 188
B.2 Chapter 2 188
B.3 Chapter 3 190
B.4 Chapter 4 192
B.5 Chapter 5 194
B.6 Chapter 6 196
Appendix C Selected Books and Reviews for Quick Reference 198
C.1 Presolar grains 198
C.2 Stellar evolution and nucleosynthesis 198
C.3 AGB stellar evolution and nucleosynthesis 199
Bibliography 200
Index 222

Meteoritic Presolar Grains And Their Significance -- Basics Of Stellar Nucleosynthesis -- Laboratory Analysis Of Presolar Grains -- The Origin Of Presolar Sic Grains -- Heavy Elements In Presolar Sic Grains -- Diamond. Graphite And Oxide Grains. Maria Lugaro. Includes Bibliographical References (p. 183-205) And Index.

One of the most fascinating discoveries of the last fifty years is that much of the materials that constitutes our world and ourselves came from the stars.

2009-07-20