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Observational Tests of the Formation, Migration, and Evolution Processes of Gas Giant Planets

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Observational Tests of the Formation, Migration, and Evolution Processes of Gas Giant Planets OBSERVATIONAL TESTS OF THE FORMATION, MIGRATION, AND EVOLUTION PROCESSES OF GAS GIANT PLANETS by Alessandro Sozzetti Laurea in Physics, University of Turin, 1997 M. S. in Physics, University of Pittsburgh, 2002 Submitted to the Graduate Faculty of the Department of Physics & Astronomy in partial fulfillment of the requirements for the degree of Doctor of Philosophy University of Pittsburgh 2005 UNIVERSITY OF PITTSBURGH DEPARTMENT OF PHYSICS & ASTRONOMY This dissertation was presented by Alessandro Sozzetti It was defended on May 25, 2005 and approved by David A. Turnshek, PhD, Professor, Physics & Astronomy David W. Latham, PhD, Senior Astronomer, Smithsonian Astrophysical Observatory Andrew J. Connolly, PhD, Assistant Professor, Physics & Astronomy Daniel Boyanovsky, PhD, Professor, Physics & Astronomy John D. Hillier, PhD, Associate Professor, Physics & Astronomy Bruce W. Hapke, PhD, Professor Emeritus, Geology & Planetary Science Dissertation Advisors: David A. Turnshek, PhD, Professor, Physics & Astronomy, David W. Latham, PhD, Senior Astronomer, Smithsonian Astrophysical Observatory ii Copyright °c by Alessandro Sozzetti 2005 iii OBSERVATIONAL TESTS OF THE FORMATION, MIGRATION, AND EVOLUTION PROCESSES OF GAS GIANT PLANETS Alessandro Sozzetti, PhD University of Pittsburgh, 2005 We have conducted a set of experiments aimed at improving our knowledge of the formation, migration, and evolution processes of gas giant planets, utilizing a combination of spectro- scopic, photometric, and astrometric techniques. First, the distributions of planet masses and orbital elements, different correlations among them, and measurable differences in planetary frequency are likely to be generated by diverse planetary formation scenarios and evolution mechanisms as well as different characteristics of the parent star (binarity, spectral type, metallicity, age). We have found new evidence for a correlation between the orbital periods of extrasolar planets and the metallicity of the host stars. We have undertaken a precision radial-velocity survey of a sample of 200 metal-poor stars, to confirm or disprove the correlation, to refine our understanding of the dependence of planetary frequency on the metallicity of the host stars, and to put constraints on proposed models of giant planet formation. Second, the internal structure and composition of the atmospheres of close-in giant plan- ets can be better understood if measurements of their radii and actual masses are available, for a range of different planet host spectral types. We have measured the spectroscopic orbit of TrES-1, the transiting Jupiter-sized planet of a moderately bright K0V star, and by im- proving on the determination of the stellar parameters, we have derived accurate estimates of its radius and mass. Finally, the actual source responsible for eccentricity excitation could be understood and the long-term dynamical evolution better characterized if coplanarity measurements iv of multiple-planet orbits were to be carried out. We have quantified the ability of the Space Interferometry Mission to obtain accurate measurements of the actual masses, orbital parameters, and relative inclination angles for systems of giant planets around stars in the solar neighborhood. We conclude describing four experiments to investigate further the transiting planet TrES-1 and its parent star. These are: 1) infrared observations of the secondary eclipse; 2) high-precision visible wavelength observations of the primary eclipse; 3) a detailed chemical abundance analysis of the host star; 4) a direct distance measurement for the system. v He, who through vast immensity can pierce, See worlds on worlds compose one universe, Observe how system into system runs, What other planets circle other suns, What varied Being peoples every star, May tell why Heaven has made us as we are. Alexander Pope An Essay on Man, 1734 TO MY FATHER. vi PREFACE Upon my arrival at the University of Pittsburgh, in August 2000, I was firmly hoping I would be able to continue to work on the topic which had monopolized my scientific interests since the early days of my undergraduate thesis research in Italy: Extrasolar planets. When I declared my intention to carry out planet-related thesis work at the Harvard- Smithsonian Center for Astrophysics, Dave Turnshek openly encouraged me to pursue it. I want to thank him for having always been a fervent supporter of all of my plans. The first time I met Dave Latham, having driven for ten hours from Pittsburgh to the town of Harvard, I was terribly late for supper. I called him along the way saying I was planning to eat somewhere in Connecticut, but he replied: “No, of course you must come here to eat it all, and have some good wine!”. Dave is a superlative host. If he tells you he will be serving good wine, you can rest assured it will be a night to remember. The wine tastings he sponsors at the Center for Astrophysics have become proverbial. It’s too bad he has such a strong French bias. In all my efforts, I have not been able to move him significantly toward the Italian border! Dave and I share many common views and have a common understanding of how many things in life work. This has obviously helped a lot in both our personal and professional interactions. But most importantly, Dave has taught me countless things. One lesson I like in particular is that one should not rush, but rather be patient, and wait until until he/she has good data, and lots of them. And, of course, Dave convinced me that I should at least be able to count up to three in Spanish: uno, dos, TrES! Willie Torres has traveled with me each and every time I had to go to Hawaii. Without his well-trained hat, we would never have gotten such a long series of good observing nights! In addition, Willie treats HIRES as a little pet, and without somebody taking such good vii care of world-class instrumentation, things would never have gone smoothly, as instead they did, all the time. He’s a great scientist, an outstanding collaborator, and a good friend, and I thank him for being all that at once. Mike Kurtz, Dimitar Sasselov, and Maciej Konacki have provided crucial advice, im- portant information, and useful discussions many times during my stay at the Center for Astrophysics. Their help is worth more than a simple word of acknowledgment! The Graduate Secretary Leyla Hirschfeld in Pittsburgh and the Division Administrator Leslie Feldman in Cambridge have been extremely helpful throughout my student career. Any time I called for aid, even over small, tiny issues, they always responded within the blink of an eye. I owe them many thanks. During graduate school, it’s easy to stick around with a bunch of school-mates while you’re working yourself through countless nasty, and sometimes pointless!, homework exer- cises. Then, when you start your thesis, you end up losing track of many of them. But, with good friends you stick around also out of office hours (even when there’s twelve of them a day). It was no stranger who hosted us in Denver, on our way to a conference, after a wonderful trip across the National Parks of the South-West. Kip, Ramin, Phil, Michele, Barun, thanks! Even after moving to Cambridge, any time I came back to Pittsburgh it was always great to see you again, and after greetings, the first thing to be said would be: “What do we do tonight?”. It’s well known that Pre-Doctoral Fellows at the CfA are looked upon by Harvard gradu- ate students with a slight hint of superiority complex. But many pre-docs are not only very good at what they do, they also are great human beings. My stay in Cambridge would not have been the same without a pizza + movie with Ettore, a well-made italian coffee with Peter, Paula, Antonio, and Rui, or a wine + cheese + cured meats tasting with Gabor, Luis, and Balasz. My family has supported my choices all along. It has not been easy, I decided to under- take a career path that was fully orthogonal to theirs. But even when they had a hard time understanding the need for a certain step (“What? Why do you need a Doctorate? Isn’t a Laurea enough?”), they always trusted I would do the right thing. I am sure they are both viii very happy now. Mario, Alberto, Davide: an ocean is not enough to separate very good friends. Our life-long friendship has given me invaluable strength. Finally, thanks to Ummi Abbas for simply being the person she is. I am a most fortunate man as I will be able to tell her so for all the days to come. This work has been supported by the University of Pittsburgh through an Andrew Mellon Pre-doctoral Fellowship and a Zaccheus Daniels Fellowship, by the Smithsonian Astrophysi- cal Observatory through an SAO Pre-doctoral Fellowship, and by the Keck PI Data Analysis Fund (JPL 1262605). ix TABLE OF CONTENTS PREFACE ......................................... vii 1.0 INTRODUCTION ................................. 1 1.1 A Historical and Philosophical Perspective ................... 1 1.2 Scientific Motivations .............................. 4 1.3 Chapter Summaries ............................... 7 2.0 EXTRA-SOLAR PLANETS: A REVIEW OF THEORY AND OBSER- VATION ....................................... 12 2.1 Introduction ................................... 12 2.2 Emerging Statistical Properties of Planetary Systems ............. 13 2.2.1 Sample Completeness and Detection Thresholds ............ 14 2.2.1.1 Doppler Spectroscopy ....................... 14 2.2.1.2 Transit Photometry ........................ 17 2.2.2 Metallicity of the Host Stars ....................... 19 2.2.3 Mass, Period & Eccentricity Distributions ................ 22 2.2.4 Correlations ................................ 25 2.2.5 Multiple Systems and Planets in Stellar Systems ............ 30 2.2.6 Follow-up Studies ............................. 33 2.2.6.1 Astrometry ............................ 33 2.2.6.2 Spectro-Photometry in the Visible ................ 35 2.2.6.3 Infrared Emission ......................... 36 2.2.6.4 Planet-Induced Chromospheric Activity and Radio Emission .
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