DOCSLIB.ORG

Investigating Planet Formation and Composition Through Observations of Carbon and Oxygen Species in Stars, Disks, and Planets

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

Connecting the Dots: Investigating Planet Formation and Composition Through Observations of Carbon and Oxygen Species in Stars, Disks, and Planets Item Type text; Electronic Dissertation Authors Teske, Johanna Kavanagh 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 26/09/2021 06:42:44 Link to Item http://hdl.handle.net/10150/318831 CONNECTING THE DOTS: INVESTIGATING PLANET FORMATION AND COMPOSITION THROUGH OBSERVATIONS OF CARBON AND OXYGEN SPECIES IN STARS, DISKS, AND PLANETS by Johanna Kavanagh Teske A Dissertation Submitted to the Faculty of the DEPARTMENT OF ASTRONOMY In Partial Fulfillment of the Requirements For the Degree of DOCTOR OF PHILOSOPHY In the Graduate College THE UNIVERSITY OF ARIZONA 2014 2 THE UNIVERSITY OF ARIZONA GRADUATE COLLEGE As members of the Dissertation Committee, we certify that we have read the dis- sertation prepared by Johanna Kavanagh Teske entitled “Connecting the Dots: Investigating Planet Formation and Composition Through Observations of Car- boy and Oxygen Species in Disks, Stars, and Planets” and recommend that it be accepted as fulfilling the dissertation requirement for the Degree of Doctor of Phi- losophy. Date: 11 April 2014 Caitlin Griffith Date: 11 April 2014 Katia Cunha Date: 11 April 2014 Simon Schuler Date: 11 April 2014 Daniel Apai Date: 11 April 2014 George Rieke Final approval and acceptance of this dissertation is contingent upon the candi- date’s submission of the final copies 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. Date: 11 April 2014 Dissertation Director: Caitlin Griffith 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 Univer- sity Library to be made available to borrowers under rules of the Library. Brief quotations from this dissertation are allowable without special permis- sion, 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 head of the major department or the Dean of the Graduate College when in his or her judgment the proposed use of the material is in the interests of scholarship. In all other instances, however, permission must be obtained from the author. SIGNED: Johanna Kavanagh Teske 4 ACKNOWLEDGMENTS I would like to acknowledge the patience, dedication, and open-minded atti- tude of my second year project and thesis advisors, Joan Najita, Caitlin Griffith, Simon Schuler, and Katia Cunha. These individuals have given me multitudes of good advice, their time and energy (a lot of it!), and helped me become a bet- ter researcher and a better person. Thanks also to my other co-authors on these thesis papers, who contributed their time and expertise to make the science pos- sible and understandable (and publishable): Dr. John Carr, Dr. Ilaria Pascucci, Dr. Daniel Apai, Dr. Thomas Henning, Jake Turner, Matthias Mallonn (formerly Mueller), and especially Dr. Verne Smith, who has been instrumental in obser- vation gathering and interpretation, and has helped me shape my postdoctoral plans. I would like to thank very much Dr. Don McCarthy, Dr. Edward Prather, Gina Brissenden, and Dr. Colin Wallace, who have helped foster my teaching and communication skills, and kept me engaged in thinking and excited about education and outreach. I would like to acknowledge the National Science Foundation for funding my first three years of graduate school, and enabling me to work with whomever I wanted during this time. I was also supported during the summer by Dr. Grif- fith’s NASA’s Planetary Atmospheres Program grant, and during this last year by a NASA Keck PI grant. In addition, my thesis was possible due to the data available in the Keck Observatory Archive (KOA), operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration, as well as data collected from the Subaru and Keck telescopes on Mauna Kea. For this I acknolwedge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. My thesis also used data collected with the STELLA robotic telescope in Tenerife, an AIP facility jointly operated by AIP and IAC, and the University of Arizona Kuiper 1.55 m telescope on Mount Bigelow. I thank the staff at all of these facilities, particularly the Kuiper Telescope, for their patience, and the University of Arizona, NOAO, and NASA TACs for awarding time for my thesis observations. 5 DEDICATION This thesis is dedicated to my dad, who took me to museums around the world, introduced me to Contact, and taught me that “doing the math” was cool; my first and second grade teacher Rick Stevens, who fostered in me the wonder of discovery and exploration; my middle school English teacher, Mrs. Ellen Flurry, who made sure I knew I could do whatever I put my mind to; my “PALTAG” teacher, Mrs. Susan Bucks, whose class and joie de vivre were my fuel through high school; my high school chemistry teacher, Mrs. Judy Iskowitz, who got me hooked on spectroscopy and understanding the physical universe; Dr. Monika Konaklieva, my college organic chemistry teacher, who let me do an extra credit project about PAHs that spurred my interest in astrochemistry; my college ad- visor, Dr. Nathan Harshman, who believed in me and was so passionate about his teaching; Dr. Jackie Milingo, my first REU advisor who introduced me to re- search and how think about constructing a research project; my friends in college and graduate school who suffered with me, believed in me, and made me laugh; and Dr. Alycia Weinberger, my undergraduate thesis advisor who jump-started my astronomy career, who has continued be a fantastic advisor and role model, and without whom I wouldn’t have made it into or through graduate school. Finally, and most importantly, I dedicate this thesis to my mom, who has been my inspiration and my rock, kept me humble and sane, always eager to hear about my life and my work, an invaluabe source of wisdom, and who believed in me when I didn’t believe in myself. 6 TABLE OF CONTENTS LIST OF FIGURES ................................ 8 LIST OF TABLES ................................. 10 ABSTRACT .................................... 11 1 INTRODUCTION ................................ 13 2 OVERVIEW OF STAR & PLANET FORMATION ................ 17 2.1 Stage1:Stars................................ 17 2.1.1 Brief Outline of Stellar/Galactic Chemical Evolution .... 17 2.1.2 MeasuringStellarComposition . 21 2.2 Stage2:Disks ............................... 28 2.2.1 Observational Constraints of Disk Physical Processes and Composition............................ 31 2.3 Stage3:Planetesimals .. .. .. .. .. .. .. 36 2.4 Stage4:Planets .............................. 38 2.4.1 Observational Constraints on Exoplanet Compositions ... 41 2.5 ConnectingtheDots–TheRoleofCandO . 45 2.5.1 Stage 0: Host Star Composition’s Role in Planet Formation . 45 2.5.2 Step1:CandOintheProtoplanetaryDisk . 47 2.5.3 Step2:CandOinPlanetesimals . 51 2.5.4 Step3:CandOinPlanets . 55 2.6 LastWord ................................. 62 3 MEASURING ORGANIC MOLECULAR EMISSION IN DISKS WITH LOW RES- OLUTION Spitzer SPECTROSCOPY ....................... 64 3.1 Introduction ................................ 65 3.2 DataSets.................................. 67 3.3 AnalysisandResults ........................... 70 3.3.1 SHvs.SLMeasurements . 70 3.3.2 VariationinHCNFeatureStrength . 80 3.4 Discussion ................................. 86 3.5 Summary&Conclusions. 90 4 OPTICAL OBSERVATIONS OF THE TRANSITING EXOPLANET GJ 1214B . 92 4.1 Introduction ................................ 93 4.2 ObservationsandDataReduction . 96 4.3 LightCurveAnalysis. .. .. .. .. .. .. .. 99 4.4 Discussion&Conclusions . 102 7 5 C/ORATIOS OF STARS WITH TRANSITING HOT JUPITER EXOPLANETS . 116 5.1 Introduction ................................117 5.1.1 TheRoleofCarbonandOxygen . 119 5.2 ObservationsandDataReduction . 121 5.3 Derivation ofStellarParametersandAbundances . 122 5.3.1 StellarAbundancesofNi,C,andO . 125 5.3.2 AbundanceUncertanties. 129 5.4 ResultsandDiscussion . 130 5.4.1 Comparison to Previous Studies of C and O in Exoplanet HostStars .............................131 5.4.2 Trends with C/Ohost star versus Planetary Parameters . 137 5.4.3 CarbonandOxygeninSpecificExoplanetSystems . 140 5.5 Summary..................................154 6 CARBON AND OXYGEN ABUNDANCES IN THE HOT JUPITER EXOPLANET HOST STAR XO-2N AND ITS BINARY COMPANION ............. 169 6.1 Introduction ................................170 6.2 ObservationsandDataReduction . 172 6.3 AbundanceAnalysisandResults . 172 6.4 Discussion .................................175 6.5 Conclusions ................................179 7 CARBON AND OXYGEN ABUNDANCES IN COOL METAL-RICH EXOPLANET HOSTS: ACASE STUDY OF THE C/O RATIO OF 55 CANCRI ........ 183 7.1 Introduction ................................184 7.2 ObservationsandAbundanceAnalysis . 186 7.2.1 Data
Recommended publications
  • Building Blocks That Fall from the Sky

    Building Blocks That Fall from the Sky

    Building blocks that fall from the sky How did life on Earth begin? Scientists from the “Heidelberg Initiative for the Origin of Life” have set about answering this truly existential question. Indeed, they are going one step further and examining the conditions under which life can emerge. The initiative was founded by Thomas Henning, Director at the Max Planck Institute for Astronomy in Heidelberg, and brings together researchers from chemistry, physics and the geological and biological sciences. 18 MaxPlanckResearch 3 | 18 FOCUS_The Origin of Life TEXT THOMAS BUEHRKE he great questions of our exis- However, recent developments are The initiative was triggered by the dis- tence are the ones that fasci- forcing researchers to break down this covery of an ever greater number of nate us the most: how did the specialization and combine different rocky planets orbiting around stars oth- universe evolve, and how did disciplines. “That’s what we’re trying er than the Sun. “We now know that Earth form and life begin? to do with the Heidelberg Initiative terrestrial planets of this kind are more DoesT life exist anywhere else, or are we for the Origins of Life, which was commonplace than the Jupiter-like gas alone in the vastness of space? By ap- founded three years ago,” says Thom- giants we identified initially,” says Hen- proaching these puzzles from various as Henning. HIFOL, as the initiative’s ning. Accordingly, our Milky Way alone angles, scientists can answer different as- name is abbreviated, not only incor- is home to billions of rocky planets, pects of this question.
  • Adaptive Optics Imaging of Circumstellar Environments

    Adaptive Optics Imaging of Circumstellar Environments

    Star Formation at High Angular Resolution IAU Symposium, Vol. 221, 2004 M. G. Burton, R. Jayawardhana & T.L. Bourke, eds. Adaptive Optics Imaging of Circumstellar Environments Daniel Apai, Ilaria Pascucci, Hongchi Wang, Wolfgang Brandner and Thomas Henning Max Planck Institute for Astronomy, Kimiqsiuhl 17., Heidelberg, Germany D-69117 Carol Grady NOAO/STIS, Goddard Space Flight Center, Code 681, NASA/GSFC, Greenbelt, MD 20771, USA Dan Potter Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA Abstract. We present results from our high-resolution, high-contrast imaging campaign targeting the circumstellar environments of young, nearby stars of different masses. The observations have been conducted using the ALFA/CA 3.5m and NACO UT4/VLT adaptive optics systems. In order to enhance the contrast we applied the methods PSF-subtraction and polarimetric differential imaging (PDI). The observations of young stars yielded the identification of numerous new companion candidates, the most interesting one being rv 0.5" from FU Ori. We also obtained high-resolution near-infrared imaging of the circumstellar envelope of SU Aur and AB Aur. Our PDI of the TW Hya circumstellar disk traced back the disk emission as close as 0.1" ~ 6 AU from the star, the closest yet. Our results demonstrate the potential of the adaptive optics systems in achieving high-resolution and high-contrast imaging and thus in the study of circumstellar disks, envelopes and companions. 1. Introduction Young, nearby stars are our prime source of information to study the circum- stellar disk structure and evolution. They are also the ideal targets for adaptive optics (AO) observations, as they are usually bright enough to provide excellent wavefront reference.
  • Route to Complex Organic Molecules in Astrophysical Environments

    Route to Complex Organic Molecules in Astrophysical Environments

    A New “Non-energetic” Route to Complex Organic Molecules in Astrophysical Environments: The C + H2O → H2CO Solid-state Reaction Alexey Potapov1, Serge Krasnokutski1, Cornelia Jäger1 and Thomas Henning2 1Laboratory Astrophysics Group of the Max Planck Institute for Astronomy at the Friedrich Schiller University Jena, Institute of Solid State Physics, Helmholtzweg 3, 07743 Jena, Germany, email: [email protected] 2Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany Abstract The solid-state reaction C + H2O → H2CO was studied experimentally following the co- deposition of C atoms and H2O molecules at low temperatures. In spite of the reaction barrier and absence of energetic triggering, the reaction proceeds fast on the experimental timescale pointing to its quantum tunneling mechanism. This route to formaldehyde shows a new “non- energetic” pathway to complex organic and prebiotic molecules in astrophysical environments. Energetic processing of the produced ice by UV irradiation leads mainly to the destruction of H2CO and the formation of CO2 challenging the role of energetic processing in the synthesis of complex organic molecules under astrophysically relevant conditions. 1 1. Introduction Understanding the reaction pathways to complex organic and prebiotic molecules at the conditions relevant to various astrophysical environments, such as prestellar cores, protostars and planet-forming disks, will provide insight in the molecular diversity during the planet formation process (Jörgensen, Belloche, & Garrod 2020). Modern astrochemical reaction networks contain thousands of reactions (see, e.g., astrochemical databases such as KIDA (http://kida.astrophy.u- bordeaux.fr/) and UDFA (http://udfa.ajmarkwick.net/)). However, these networks are very sensitive to inclusions of new reactions.
  • The Remarkable Solar Twin HIP 56948: a Prime Target in the Quest for Other

    The Remarkable Solar Twin HIP 56948: a Prime Target in the Quest for Other

    Astronomy & Astrophysics manuscript no. keck56948˙2012˙04˙06 c ESO 2018 October 30, 2018 The remarkable solar twin HIP 56948: a prime target in the quest for other Earths ⋆ Jorge Mel´endez1, Maria Bergemann2, Judith G. Cohen3, Michael Endl4, Amanda I. Karakas5, Iv´an Ram´ırez4,6, William D. Cochran4, David Yong5, Phillip J. MacQueen4, Chiaki Kobayashi5⋆⋆, and Martin Asplund5 1 Departamento de Astronomia do IAG/USP, Universidade de S˜ao Paulo, Rua do Mat˜ao 1226, Cidade Universit´aria, 05508-900 S˜ao Paulo, SP, Brazil. e-mail: [email protected] 2 Max Planck Institute for Astrophysics, Postfach 1317, 85741 Garching, Germany 3 Palomar Observatory, Mail Stop 105-24, California Institute of Technology, Pasadena, California 91125, USA 4 McDonald Observatory, The University of Texas at Austin, Austin, TX 78712, USA 5 Research School of Astronomy and Astrophysics, The Australian National University, Cotter Road, Weston, ACT 2611, Australia 6 The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA Received ...; accepted ... ABSTRACT Context. The Sun shows abundance anomalies relative to most solar twins. If the abundance peculiarities are due to the formation of inner rocky planets, that would mean that only a small fraction of solar type stars may host terrestrial planets. Aims. In this work we study HIP 56948, the best solar twin known to date, to determine with an unparalleled precision how similar is to the Sun in its physical properties, chemical composition and planet architecture. We explore whether the abundances anomalies may be due to pollution from stellar ejecta or to terrestrial planet formation.
  • CURRICULUM VITAE for DANIEL APAI Research Interests: Extrasolar Planets; Planet Formation; Planetary Atmospheres; Astrobiology; Space Telescope Architectures

    CURRICULUM VITAE for DANIEL APAI Research Interests: Extrasolar Planets; Planet Formation; Planetary Atmospheres; Astrobiology; Space Telescope Architectures

    CURRICULUM VITAE FOR DANIEL APAI Research Interests: Extrasolar Planets; Planet formation; Planetary atmospheres; Astrobiology; Space telescope architectures Professional Appointments 2017 – Associate Professor, Depts. of Astronomy and Planetary Sciences, Univ. of Arizona 2011 – 2017 Assistant Professor, Depts. of Astronomy and Planetary Sciences, Univ. Arizona 2008 – 2011 Assistant Astronomer, Space Telescope Science Institute Education 2004 PhD, University of Heidelberg and Max Planck Institute of Astronomy 2000 MSc in Physics, University of Szeged Recent International Service: Chair, HST–TESS Advisory Committee, Space Telescope Science Institute Science Advisory Committee member, Giant Magellan Telescope Executive Committee member, NASA Exoplanet Program Analysis Group (EXOPAG) Steering Committee member, NASA Nexus for Exoplanet System Science (NExSS) Chair, Exoplanet Science Questions for Direct Imaging Missions, SAG15/EXOPAG Member, Hubble Space Telescope Financial Review Committee Major Approved Programs as Principal Investigator 9 Hubble Space Telescope + 4 Spitzer Space Telescope programs, including: - Extrasolar Storms: Spitzer Exploration Science Program (1,144 Spitzer hour, 24 HST orbits) - Cloud Atlas: Hubble Space Telescope (112 orbits), 12+ refereed papers Earths in Other Solar Systems: $5.7M program (R&A), 45-member team, 140 refereed papers Nautilus: A large-aperture space telescope for a biosignature survey based on diffractive optics, Co-PI of $1.1M Gordon & Betty Moore Foundation grant Advising/Mentoring: Postdoc. Researchers
  • Peter Plavchan

    Peter Plavchan

    Peter Plavchan Assistant Professor of Astronomy Associate Director, George Mason Observatory PI, EarthFinder NASA Mission Concept Study PI, Astrophysics of Exoplanets Instrumentation Lab Co-PI, MINERVA-Australis Department of Physics & Astronomy Office: (703) 903-5893 George Mason University Cell: (626) 234-1628 Planetary Hall 263 Fax: (703) 993-1269 4400 University Dr, MS 3F3 [email protected] Fairfax, VA 22030 http://exo.gmu.edu twitter:@PlavchanPeter Education University of California, Los Angeles, Los Angeles, CA 2001-2006 MS, PhD in Physics California Institute of Technology, Pasadena, CA 1996-2001 BS in Physics, with honor Awards & Honors College of Science Excellence in Mentoring award nomination 2019 College of Natural and Applied Sciences Research Award, MSU 2017 NASA Group Achievement Award 2017 Citation: For the development and tests at Mauna Kea observatories of a near-infrared Laser Frequency Comb as a wavelength standard for the detection and characterization of exoplanets. NASA Honor Achievement Award, NASA Exoplanet Archive Team 2014 Citation: For outstanding achievement in the rapid and on-budget launch of the NASA Exoplanet Archive NASA Honor Achievement Award, Spitzer Science In-Reach Team 2010 Citation: For outstanding support of Spitzer IRAC Warm Instrument Characterization and significant contributions to NASA and JPL commitments to education of the global community. UCLA Physics Division Fellowship 2001-2006 Kobe International School of Planetary Sciences Fellowship 2005 Astronomy Department Outstanding Teaching
  • The Interstellar and Circumnuclear Medium of Active Nuclei Traced by H I 21 Cm Absorption

    The Interstellar and Circumnuclear Medium of Active Nuclei Traced by H I 21 Cm Absorption

    The Astronomy and Astrophysics Review (2018) 26:4 https://doi.org/10.1007/s00159-018-0109-x REVIEW ARTICLE The interstellar and circumnuclear medium of active nuclei traced by H i 21 cm absorption Raffaella Morganti1,2 · Tom Oosterloo1,2 Received: 23 April 2018 © The Author(s) 2018 Abstract This review summarises what we have learnt in the last two decades based on H i 21 cm absorption observations about the cold interstellar medium (ISM) in the central regions of active galaxies and about the interplay between this gas and the active nucleus (AGN). Hi absorption is a powerful tracer on all scales, from the parsec-scales close to the central black hole to structures of many tens of kpc tracing interactions and mergers of galaxies. Given the strong radio continuum emission often associated with the central activity, H i absorption observations can be used to study the Hi near an active nucleus out to much higher redshifts than is possible using H i emission. In this way, Hi absorption has been used to characterise in detail the general ISM in active galaxies, to trace the fuelling of radio-loud AGN, to study the feedback occurring between the energy released by the active nucleus and the ISM, and the impact of such interactions on the evolution of galaxies and of their AGN. In the last two decades, significant progress has been made in all these areas. It is now well established that many radio loud AGN are surrounded by small, regularly rotating gas disks that contain a significant fraction of H i.
  • Hubble Space Telescope Primer for Cycle 18

    Hubble Space Telescope Primer for Cycle 18

    January 2010 Hubble Space Telescope Primer for Cycle 18 An Introduction to HST for Phase I Proposers Space Telescope Science Institute 3700 San Martin Drive Baltimore, Maryland 21218 [email protected] Operated by the Association of Universities for Research in Astronomy, Inc., for the National Aeronautics and Space Administration How to Get Started If you are interested in submitting an HST proposal, then proceed as follows: • Visit the Cycle 18 Announcement Web page: http://www.stsci.edu/hst/proposing/docs/cycle18announce Then continue by following the procedure outlined in the Phase I Roadmap available at: http://apst.stsci.edu/apt/external/help/roadmap1.html More technical documentation, such as that provided in the Instrument Handbooks, can be accessed from: http://www.stsci.edu/hst/HST_overview/documents Where to Get Help • Visit STScI’s Web site at: http://www.stsci.edu • Contact the STScI Help Desk. Either send e-mail to [email protected] or call 1-800-544-8125; from outside the United States and Canada, call [1] 410-338-1082. The HST Primer for Cycle 18 was edited by Francesca R. Boffi, with the technical assistance of Susan Rose and the contributions of many others from STScI, in particular Alessandra Aloisi, Daniel Apai, Todd Boroson, Brett Blacker, Stefano Casertano, Ron Downes, Rodger Doxsey, David Golimowski, Al Holm, Helmut Jenkner, Jason Kalirai, Tony Keyes, Anton Koekemoer, Jerry Kriss, Matt Lallo, Karen Levay, John MacKenty, Jennifer Mack, Aparna Maybhate, Ed Nelan, Sami-Matias Niemi, Cheryl Pavlovsky, Karla Peterson, Larry Petro, Charles Proffitt, Neill Reid, Merle Reinhart, Ken Sembach, Paula Sessa, Nancy Silbermann, Linda Smith, Dave Soderblom, Denise Taylor, Nolan Walborn, Alan Welty, Bill Workman and Jim Younger.
  • HIGH PRECISION ABUNDANCES of the OLD SOLAR TWIN HIP 102152: INSIGHTS on LI DEPLETION from the OLDEST SUN* Talawanda R

    HIGH PRECISION ABUNDANCES of the OLD SOLAR TWIN HIP 102152: INSIGHTS on LI DEPLETION from the OLDEST SUN* Talawanda R

    Published in ApJL. Preprint typeset using LATEX style emulateapj v. 04/17/13 HIGH PRECISION ABUNDANCES OF THE OLD SOLAR TWIN HIP 102152: INSIGHTS ON LI DEPLETION FROM THE OLDEST SUN* TalaWanda R. Monroe1, Jorge Melendez´ 1, Ivan´ Ram´ırez2, David Yong3, Maria Bergemann4, Martin Asplund3, Jacob Bean5, Megan Bedell5, Marcelo Tucci Maia1, Karin Lind6, Alan Alves-Brito3, Luca Casagrande3, Matthieu Castro7, Jose{Dias´ do Nascimento7, Michael Bazot8, and Fabr´ıcio C. Freitas1 Published in ApJL. ABSTRACT We present the first detailed chemical abundance analysis of the old 8.2 Gyr solar twin, HIP 102152. We derive differential abundances of 21 elements relative to the Sun with precisions as high as 0.004 dex (.1%), using ultra high-resolution (R = 110,000), high S/N UVES spectra obtained on the 8.2-m Very Large Telescope. Our determined metallicity of HIP 102152 is [Fe/H] = -0.013 ± 0.004. The atmospheric parameters of the star were determined to be 54 K cooler than the Sun, 0.09 dex lower in surface gravity, and a microturbulence identical to our derived solar value. Elemental abundance ratios examined vs. dust condensation temperature reveal a solar abundance pattern for this star, in contrast to most solar twins. The abundance pattern of HIP 102152 appears to be the most similar to solar of any known solar twin. Abundances of the younger, 2.9 Gyr solar twin, 18 Sco, were also determined from UVES spectra to serve as a comparison for HIP 102152. The solar chemical pattern of HIP 102152 makes it a potential candidate to host terrestrial planets, which is reinforced by the lack of giant planets in its terrestrial planet region.
  • Astronomy 2008 Index

    Astronomy 2008 Index

    Astronomy Magazine Article Title Index 10 rising stars of astronomy, 8:60–8:63 1.5 million galaxies revealed, 3:41–3:43 185 million years before the dinosaurs’ demise, did an asteroid nearly end life on Earth?, 4:34–4:39 A Aligned aurorae, 8:27 All about the Veil Nebula, 6:56–6:61 Amateur astronomy’s greatest generation, 8:68–8:71 Amateurs see fireballs from U.S. satellite kill, 7:24 Another Earth, 6:13 Another super-Earth discovered, 9:21 Antares gang, The, 7:18 Antimatter traced, 5:23 Are big-planet systems uncommon?, 10:23 Are super-sized Earths the new frontier?, 11:26–11:31 Are these space rocks from Mercury?, 11:32–11:37 Are we done yet?, 4:14 Are we looking for life in the right places?, 7:28–7:33 Ask the aliens, 3:12 Asteroid sleuths find the dino killer, 1:20 Astro-humiliation, 10:14 Astroimaging over ancient Greece, 12:64–12:69 Astronaut rescue rocket revs up, 11:22 Astronomers spy a giant particle accelerator in the sky, 5:21 Astronomers unearth a star’s death secrets, 10:18 Astronomers witness alien star flip-out, 6:27 Astronomy magazine’s first 35 years, 8:supplement Astronomy’s guide to Go-to telescopes, 10:supplement Auroral storm trigger confirmed, 11:18 B Backstage at Astronomy, 8:76–8:82 Basking in the Sun, 5:16 Biggest planet’s 5 deepest mysteries, The, 1:38–1:43 Binary pulsar test affirms relativity, 10:21 Binocular Telescope snaps first image, 6:21 Black hole sets a record, 2:20 Black holes wind up galaxy arms, 9:19 Brightest starburst galaxy discovered, 12:23 C Calling all space probes, 10:64–10:65 Calling on Cassiopeia, 11:76 Canada to launch new asteroid hunter, 11:19 Canada’s handy robot, 1:24 Cannibal next door, The, 3:38 Capture images of our local star, 4:66–4:67 Cassini confirms Titan lakes, 12:27 Cassini scopes Saturn’s two-toned moon, 1:25 Cassini “tastes” Enceladus’ plumes, 7:26 Cepheus’ fall delights, 10:85 Choose the dome that’s right for you, 5:70–5:71 Clearing the air about seeing vs.
  • EOS Newsletter May 2019

    EOS Newsletter May 2019

    PROJECT EOS May 24, 2019 EARTHS IN OTHER SOLAR SYSTEMS Recent Publications On the Mass Function, Multiplicity, and Origins of Wide-Orbit Giant Planets ………………………………. Unlocking CO Depletion in PROJECT EOS Protoplanetary Disks II. Primordial C/H Predictions Inside the CO Snowline ……………………………….. Laboratory evidence for co- condensed oxygen- and carbon-rich meteoritic is part of NASA’s Nexus for stardust from nova outbursts Earths in Other Solar Systems Exoplanetary System Science program, which carries out ……………………………….. coordinated research toward to the goal of searching for and + Line Ratios Reveal N2H determining the frequency of habitable extrasolar planets with Emission Originates above the atmospheric biosignatures in the Solar neighborhood. Midplane in TW Hydrae Our interdisciplinary EOS team includes astrophysicists, ……………………………….. planetary scientists, cosmochemists, material scientists, No Clear, Direct Evidence for chemists and physicists. Multiple Protoplanets The Principal Investigator of EOS is Daniel Apai (University of Orbiting LkCa 15: LkCa 15 Arizona). The project’s lead institutions are The University of bcd are Likely Inner Disk Arizona‘s Steward Observatory and Lunar and Planetary Signals Laboratory. ……………………………….. The EOS Institutional Consortium consists of the Steward The Exoplanet Population Observatory and the Lunar and Planetary Laboratory of the Observation Simulator. II - University of Arizona, the National Optical Astronomy Population Synthesis in the Observatory, the Department of Geophysical Sciences at the Era of Kepler University of Chicago, the Planetary Science Institute, and the Catholic University of Chile. For a complete list of publications, please visit the EOS Library on the SAO/NASA Astrophysics Data System. eos-nexus.org !1 PROJECT EOS May 24, 2019 On the Mass Function, Multiplicity, and Origins of Wide-Orbit Giant Planets Kevin Wagner, Dániel Apai, Kaitlin M.
  • EOS Newsletter MARCH 2020

    EOS Newsletter MARCH 2020

    PROJECT EOS March 15, 2020 EARTHS IN OTHER SOLAR SYSTEMS Recent Publications ACCESS: A Visual toNear-infrared Spectrum of the Hot Jupiter WASP-43b with Evidence of H2O, but No Evidence of Na or K ………………………………. Identifying Exo-Earth Candidates in Direct Imaging Data through PROJECT EOS Bayesian Classification ………………………………. Nautilus: A Very Large-Aperture, Ultralight Space Telescope for Exoplanet Exploration, Time- domain Astrophysics, and Faint Objects ………………………………. EPOS: Exoplanet Population Earths in Other Solar Systems is part of NASA’s Nexus for Observation Simulator Exoplanetary System Science program, which carries out ……………………………….. coordinated research toward to the goal of searching for and ACCESS: the Arizona-CfA- determining the frequency of habitable extrasolar planets with Catolica-Carnegie Exoplanet atmospheric biosignatures in the Solar neighborhood. Spectroscopy Survey Our interdisciplinary EOS team includes astrophysicists, ……………………………….. Exoplanet Population Synthesis in planetary scientists, cosmochemists, material scientists, the Era of Large Exoplanets chemists and physicists. Surveys The Principal Investigator of EOS is Daniel Apai (University of ……………………………….. Arizona). The project’s lead institutions are The University of The Sun-like Stars Opportunity ……………………………….. Arizona‘s Steward Observatory and Lunar and Planetary Life Beyond the Solar System: Laboratory. Remotely Detectable The EOS Institutional Consortium consists of the Steward Biosignatures Observatory and the Lunar and Planetary Laboratory of the ……………………………….. Planet formation and migration University of Arizona, the National Optical Astronomy near the silicate sublimation front Observatory, the Department of Geophysical Sciences at the in protoplanetary disks University of Chicago, the Planetary Science Institute, and the ……………………………….. Catholic University of Chile. Search for L5 Earth Trojans with For a complete list of publications, please visit the DECam EOS Library on the SAO/NASA Astrophysics Data System.