The distribution of water in the solar nebula: Implications for solar system formation Item Type text; Dissertation-Reproduction (electronic) Authors Cyr, Kimberly Ellen, 1964- Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 01/10/2021 06:46:45 Link to Item http://hdl.handle.net/10150/288870 INFORMATION TO USERS This manuscript has been reproduced from the microfilm master. UMI films the text directly from the original or copy submitted. Thus, some thesis and dissertation copies are in typewriter face, while others may be from any type of computer printer. The quality of this reproduction is dependent upon the quality of the copy submitted. 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Contact UMI directly to order. UMI A Bell & Howell Information Company 300 North Zeeb Road, Ann Arbor MI 48106-1346 USA 313/761-4700 800/521-0600 THE DISTRIBUTION' OF WATER IN THE SOLAR NEBULA: IMPLICATION'S FOR SOLAR SYSTEM FORMATION b_\- Kimberly Ellen Cyr Copyright © Kimberly Ellen Cyr 1998 A Dissertation Submitted to the Faculty of the DEPARTMENT OF PLANETARY SCIENCES In Partial Fulfillment of the Requirements For the Degree of DOCTOR OF PHILOSOPHY In the Graduate College THE UNIVERSITY OF ARIZONA 1 9 9 S DMI Number: 9901693 Copyright 199 8 by Cyr, Kimberly Ellen All rights reserved. UMI Microform 9901693 Copyright 1998, by UMI Company. All rights reserved. This microform edition is protected against unauthorized copying under Title 17, United States Code. UMI 300 North Zeeb Road Ann Arbor, MI 48103 THE UNIVERSITY OF ARIZONA ® GRADUATE COLLEGE As members of the Final Examination Committee, we certify that we have read the dissertation prepared by Kimberly Ellen Cyr entitled The Distribution of Water in the Solar Nebula: Implications for Solar System Formation and recommend chat it be accepted as fulfilling the dissertation requirement for the Degree of Doctor of Philosophy un I ne Date d^<rT(h-- Date Date Chris Chyba Date Date Final approval and acceptance of this dissertation is contingent upon the candidate's submission of the final copy of the dissertation to the Graduate College. I hereby certify that I have read this dissertation prepared under my direction and recommend that it be accepted as fulfilling the dissertation requirement. 3 STATEMENT BY AUTHOR This dissertation has been submitted in partial fulfillment of requirements for an advanced degree at The University of Arizona and is deposited in the I'ni- versity Library to be made available to borrowers under rules of the library. Brief quotations from this dissertation are allowable without special per­ mission, provided that accurate acknowledgment of source is made. Requests for permission for extended quotation from or reproduction of this manuscript in whole or in part may be granted by the copyright holder. SIGNED: 4 ACKNOWLEDGEMENTS This work was supported in part by N'ASA GSRP grants XGT-oir27 and XGT- 51646. and the N.\SA Origins program. In the course of my graduate career I have also been supported by various people in various ways, and I'd like to briefly highlight some of them. Chief among them are my family, who has always given me their support and encouragement: and my advisor. .Jonathan Lunine. who has given me his patience, support and scientific e.xpertise and guidance. I would also like to mention Faith Vilas, of Johnson Space Center, who was the first to suggest LPL to me for grad school and sent me out to visit the department, and who has always been a mentor to and indefatiguable supporter of me. Further. I have been lucky to have chosen my grad school wisely in that I ended up in a great community of grad students. These people have been housemates, friends and some of the nicest and most fun. if sometimes totally bizarre, peo­ ple I've known. First. I have managed to live at Hawthorne House for my entire grad career, through leaky roofs, generations of stray cats giving birth in our shed, power outages, monsoons, repainting, summer power bills, desert insects, innumer­ able Bratfests and other parties, and many Thanksgiving. Christmas. .New Year's. Passover and Easter celebrations. 1 have occasionally been asked how or why 1 lasted so long at HH. and the answer has always been mostly because of the people, my fellow housemates. In no particular order, these include Mike and Ellen, their dogs Tasha and Zephyr. Bill Bottke. Andy Rivkin—the housemate who was with me the longest, and still a good friend. Doyle Hall—who brightened my days then, as he continues to do now. John Stansberry. Cynthia Phillips. Bob Reid. Laszlo Keszthelyi. Joe Spitale and Rachel Mastrapa. Second, in addition to my housemates, my circle of grad school friends also included Erik; Will; Kevin; fellow movie-afficionado Mark; my officemates and friends Zibi and Barb; classmates Seran (and .\Ia.x). Jim. William and Betty: Jen; Doug; Ron: the truly warped but always hilarious and ever helpful Chris Schaller. and the equally-but-difFerently funny and warped Dave Trilling, among others. I would be remiss if I did not also mention some of the other friendships I've made while in grad school including those with people in the local and online dance communities, especially Jan: and those with several other people who were with me through some of the tougher and more profound moments including Catherine. Katherine. .Melanie and most especially Sharon—who has been a teacher and guide as well as a friend. .Many thanks to all! •5 DEDICATION "7 rtalizt this was not exactly the kind of grad career you had in mind, but it's the one you got. Maybe that 's because it was the one you needed. ~ To all things seen and unseen. 6 TABLE OF CONTENTS LIST OF FIGURES 9 LIST OF TABLES 10 ABSTRACT 11 1 INTRODUCTION 13 2 THE SOLAR NEBULA 17 2.1 Introduction IT 2.2 Overview of Formation and Evolution IS 2.3 Modeling 21 2.1 Nebular .Models Used in this Work 26 2.5 Complicating Factors -JO 2.5.1 .Nebular Opacity Changes 30 2.5.2 Protostellar Temperature and .Mass Changes 31 2.5.3 Gas .Motions 32 2.5.4 Gravitational Instability 37 2.5.5 Episodic Thermal Phenomena 39 2.5.6 .Migrating Giant Planets 42 2.6 Timing: Pertinent .N'ebula Stages 44 2.7 Summary 46 3 GAS DRAG-INDUCED RADIAL DRIFT 47 3.1 Introduction 47 3.2 Model 48 3.2.1 Gas Drag 48 3.2.2 .Nebular .Model 50 3.2.3 Drift .Model 52 3.3 Results 54 3.3.1 Crystalline Ice 54 3.3.2 .Vmorphous Ice 60 3.3.3 Effects of Other .Nebular Processes 62 3.4 Summary 62 TABLE OF CONTESTS — Continued 4 DIFFUSION AND DRIFT 64 4.1 Introduction 64 4.2 Model 6o 4.2.1 .Numerical Model 6-5 4.2.2 Source Terms 66 4.2.3 Grain Growth Rates and Other Timescales 67 4.3 Diffusion Results 69 4.4 Effects of Other Nebula Processes 74 4.4.1 .\dvective Gas Flows 74 4.4.2 Migrating Planets 76 4.4.3 Lightning 78 4.4.4 FU Orionis Bursts 78 4.0 Summary 79 5 NEBULAR CHEMISTRY 82 •5.1 Introduction 82 0.2 Chemical-Dynamical .Models 83 •5.2.1 General Framework 83 0.2.2 C. H. .\. O Chemistry 8-5 0.3 Chemical Equilibrium Calculations 89 0.3.1 Model 89 5.3.2 Results 94 0.3.3 Effects of Other .\ebula Processes 112 5.4 Summary 113 6 IMPLICATIONS FOR SOLAR SYSTEM BODIES 116 6.1 Introduction 116 6.2 Terrestrial Planets 117 6.3 Outer Solar System Bodies 118 6.4 .\steroids 120 6.4.1 Hydration Features 120 6.4.2 Darkening 122 6.5 Meteorites 123 6.5.1 General 123 6.5.2 Chondrules 125 6.5.3 Enstatite Chondrites 126 6.6 E.xtrasolar Planetary Systems 129 6.7 Summary 1.30 7 CONCLUSIONS 132 APPENDIX A 136 TABLE OF CONTESTS — Continued APPENDIX B REFERENCES 9 LIST OF FIGURES 2.1 Nebula Schematic 20 3.1 Radial drift velocities vs. particle size -51 3.2 Particle size vs. Time, hot nebula 55 3.3 Particle size vs. R. hot nebula 56 3.4 Particle size vs. Time, cool nebula 57 3.5 Particle size vs. R, cool nebula 58 3.6 Particle size vs. R, amorphous ice 61 4.1 Diffusion model results assuming no significant radial drift 70 4.2 Diffusion model with radial drift, hot nebula 72 4.3 Diffusion model with radial drift, cool nebula 73 5.1 Condensation sequence: 100% solar O 95 5.2 Condensation sequence: 839c solar O 99 5.3 Condensation sequence: 749c solar O 100 5.4 Condensation sequence: 669^ solar O 101 5.5 Condensation sequence: 619^ solar O 102 5.6 Condensation sequence: 579^ solar O 103 5.7 Condensation sequence; 409( solar O 106 5.8 Condensation sequence: 209? solar O 107 5.9 Condensation sequence: 109? solar 0 108 5.10 Condensation sequence: solar O 109 B.l Condensation sequence: 1009c solar 0.