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Search for Planets in Eclipsing Binary Systems

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Search for Planets in Eclipsing Binary Systems הפקולטה למדעים מדויקים RAYMOND AND BEVERLY SACKLER "ע ש ריימונד ובברלי סאקלר FACULTY OF EXACT SCIENCES בית הספר לפיסיקה ול אסטרונומיה SCHOOL OF PHYSICS & ASTRONOMY SEARCH FOR PLANETS IN ECLIPSING BINARY SYSTEMS Submitted towards the degree "Doctor of Philosophy" by Aviv Ofir The research was carried out under the supervision of Prof. Artie Hatzes (TLS, Germany) and Prof. Sara Beck Submitted to the Senate of Tel Aviv University December 2010 This is my quest, to follow the star No matter how hopeless, no matter how far To fight for the right, without question or pause To be willing to march into hell for a heavenly cause And I know, if I'll only be true to the glorious quest That my heart lies peaceful and calm When I'm laid to my rest And the world will be better for this That one man scorned and covered with scars Still strove with his last dance of courage To reach the unreachable star Extract from: "The Impossible Dream" by Mitch Leigh and Joe Darion With special credit to performance by Carter USM − I − − II − Abstract Bound binary stars are one of the most common environments in the Galaxy. Studying planet formation and evolution without including the formation and evolution of planets in binary star systems is surely incomplete. Planets are already known to readily form in wide binaries despite serious observational biases against such detections: at least 17% of the known exoplanets are known to revolve around one component of a wide binary. On the other hand, planet formation in tight binaries remain poorly constrained. This research program aimed to fill-in observational data on these types of systems. Planetary transits surveys, both ground- and space- based, collect huge amounts of photometric data that also include many eclipsing binaries (EBs). Since planets in EB systems are expected to be (at least initially) co-planar with the host binary, I used the alignment of EBs with the line of sight (by their pre-selection as eclipsing) to enhance the geometrical probability of planets in the system to transit any of the binary components. I used photometric data mainly from the CoRoT space mission. I started from the raw photometry and de-trended it to remove all sources of systematic noise. I elaborate on a special technique developed during this work called "SARS" that allowed me to clean the data enough to detect many transit-like signals in the data that were not previously detected. For variable stars, like EBs, I show how to de-trend the data while not removing the intrinsic variability. I also describe a novel searching algorithm developed during this work called "CB-BLS" to look for planets in the EB systems using the refined data. All this allows me to search for planets in almost every possible configuration: transiting planets around either or both components, non-transiting planets around both components, transiting planets in background objects, and – as a (very successful) by-product – improved searches for "regular" transiting planets around single stars. In this thesis I present the first significant results of the research program, including the detection of four transiting planets, a transiting brown dwarf, and the detection of background and eclipse timing signals. Those are just preliminary results: this research program will extend beyond the scope of this thesis and into my future postdoc, so that by the end of the program I will be able to empirically compare planet formation rate in close binaries to that of planets around single stars, thus providing a significant constraint to theories of star and planet formation, one that does not exist today. − III − Acknowledgements Some parts of these studies were not easy on me, not at all. For this reason completing this PhD thesis gives me great satisfaction. However, I myself could not rise to this challenge on my own, and I thank the following for making this possible: First and foremost – my dearest, my wife Michaela : in great storms you were my anchor, in great darkness you were my light. When I wanted you gave me space, and when I needed you gave me a hug. This could not have possibly succeeded without you. "Thank you" can't quite say it, so I plan to spend the rest of my life with you to try to find the way that does. I wish to thank my advisors - prof. Artie Hatzes and prof. Sara Beck : Artie : thank you for your warm and positive attitude, for showing uncommon trust and openness, for your time and efforts. Thank you for allowing me to work with you. Sara : thank you for making possible for me – yet again – to explore the science question I find the most intriguing, even if means confusing bureaucracy and venturing out of the TAU faculty. I wish to thank my main collaborators during this thesis - the CoRoT Exoplanets Science Team in general, and the CoRoT detection team in particular. Special thanks are due to Eike Gunther , Pierre Barge , Hans Deeg and Claud Lacy who played pivotal roles in my entry into these wonderfully collaborative teams. Last, but certainly not least – my family: quite literally, I really couldn't reach this point in my life without you. Thank you Mom for your love, time and encouragement. Thank you Dad and Rivka for your support, knowledge and faith in me. I hope that making you all proud is the best way of saying thank you, from the bottom of my heart. − IV − Table of Contents ABSTRACT ..............................................................................................................................III ACKNOWLEDGEMENTS .......................................................................................................... IV TABLE OF CONTENTS ...............................................................................................................V PART 1: INTRODUCTION TO PUBLISHED PAPERS .......................................1 1. EXOPLANETS AROUND SINGLE STARS ..........................................................................2 1.1. PRIMER ON EXOPLANETS THEORY ................................................................................2 1.2. INPUT DATA .....................................................................................................................6 1.3. DETECTION TECHNIQUES ...............................................................................................7 1.3.1. RADIAL VELOCITY (RV)............................................................................................7 1.3.2. TRANSITS ...................................................................................................................8 1.3.3. MICROLENSING ........................................................................................................11 1.3.4. DIRECT IMAGING ......................................................................................................13 1.3.5. TIMING VARIATIONS ................................................................................................17 1.3.6. ASTROMETRY ...........................................................................................................17 1.4. CHARACTERIZATION OF EXOPLANETS ........................................................................19 1.4.1. HIGH -PRECISION PHOTOMETRY ...............................................................................20 1.4.2. SPECTRA OF EXOPLANETS ........................................................................................25 1.4.3. THE ROSSITER -MCLAUGHLIN (RM) EFFECT ...........................................................26 2. EXOPLANETS AND BINARY STARS ................................................................................27 2.1. PRELUDE ........................................................................................................................27 2.1.1 . DEFINITIONS AND BIASES ........................................................................................27 2.1.2. MOTIVATION : WHAT CAN BE LEARNED FROM PLANETS IN BINARIES ? ....................28 2.2 . PREVIOUS STUDIES .................................................................................................... 30 2.2.1 . THEORETICAL STUDIES ............................................................................................30 2.2.2 . OBSERVATIONAL STUDIES .......................................................................................31 2.3 . LOOKING FOR PLANETS IN BINARIES IN THIS STUDY ............................................ 34 2.3.1 . DE-TRENDING ...........................................................................................................34 2.3.2 . S-TYPE ORBIT ...........................................................................................................36 2.3.3 . P-TYPE ORBIT ...........................................................................................................36 2.3.3.1 . MODELING ............................................................................................................ 36 2.3.3.2 . TRANSIT DETECTION – CIRCULAR ORBIT .............................................................. 37 2.3.3.3 . TRANSIT DETECTION – ECCENTRIC ORBIT ............................................................. 38 2.3.3.4 . ECLIPSE TIMING ..................................................................................................... 41 2.3.4 . BACKGROUND OBJECTS ...........................................................................................42 2.4. SERENDIPITOUS DISCOVERY .........................................................................................43
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