DOCSLIB.ORG

Eric Mamajek's Curriculum Vitae

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Eric Mamajek's Curriculum Vitae Eric E. Mamajek Curriculum Vitae - 1 February 2012 Associate Astronomer Ph. (+56) 51-205-294 National Optical Astronomy Observatory Ph. (+56) 51-205-200 x294 Cerro Tololo Inter-American Observatory Ph. (412) 467-6941 Casilla 603 - La Serena - Chile FAX: (+56) 51-205-212 http://www.ctio.noao.edu/noao/content/eric-mamajek email: [email protected] Born: 22 October 1975. Pittsburgh, Pennsylvania, USA Education 2004 Ph.D. The University of Arizona, Astronomy Thesis: “The Identification and Characterization of Young, Nearby, Solar-Type Stars” 2001 M.S. The University of Arizona, Astronomy 2000 M.Sc. The University of New South Wales, ADFA, Physics 1998 B.S. The Pennsylvania State University, Astronomy & Astrophysics, Physics 1993 H.S. Bethel Park Sr. High School Positions 2011- Associate Astronomer, Cerro Tololo Inter-American Observatory 2008-2011 Assistant Professor, Physics & Astronomy, University of Rochester 2004-2008 Clay Postdoctoral Fellow, Harvard-Smithsonian Center for Astrophysics 2000-2004 Graduate Research Assistant, University of Arizona, Astronomy 1999-2000 Graduate Teaching Assistant, University of Arizona, Astronomy 1998-1999 J. William Fulbright Fellow, Australia, ADFA/UNSW School of Physics Research Interests • Formation and Evolution of Stars, Planets, Circumstellar and Circumplanetary Disks. • Ages, Kinematics, Rotation, and Activity of Nearby Stars and Members of Star Clusters. Fellowships 2004-2008 Clay Postdoctoral Fellowship - Harvard-Smithsonian Center for Astrophysics (first ever 1st-time postdoc accepted as Clay Fellow) 2004 Hubble Postdoctoral Fellowship (declined) 2004 Michigan Society of Fellows Postdoctoral Fellowship - U. Michigan (declined) 2004 Henry Norris Russell Postdoctoral Fellowship - Princeton (declined) 2004 5-year NOAO Science Fellowship (declined) 2002-2004 NASA Graduate Student Researchers Program Fellowship 1998-1999 Fulbright Fellowship - Australia Research Grants and Awards 2011 PI, NSF-AST REU supplement, “Chemical Self-Enrichment in the Nearest OB Association” – $6.8k 2010 PI, NSF-AST, “Chemical Self-Enrichment in the Nearest OB Association” – $481k 2010 co-I, Herschel OT1, “Tracing Remnant Gas in Planet Forming Debris Disks: Confronting Theories of Ice-Giant Planet Formation” (PI V. Geers) – $14k(UR: $7k) 2009 co-I, NASA ADP, “A Photometry Catalog of Stars within 130 pc Serendipitously Observed by Spitzer”, NASA (PI D. Hines) – $186k (UR: $36k) 2007 PI, Spitzer Cycle 4, “Search for Terrestrial Temperature Debris Around Needles in the Haystack: A Survey for Disks in a New Nearby 20 Myr Old Association”, NASA – $65k 2005 co-I, Spitzer Cycle 2, “Circumstellar Disk Evolution Across the Stellar Mass Spectrum in the Upper Sco Association”, NASA (PI J. Carpenter) – $340k 2004 Clay Postdoctoral Fellowship, SAO 2002 Graduate Student Researchers Program, NASA (PI; advisor M. Meyer) – $48k 2000 Grant-in-Aid Award, Sigma Xi Scientific Research Society (PI) – $2k 1998 Fulbright Fellowship – $25k Proposals Pending or Not Selected 2011 PI, “Origins of Mini-Solar Systems”, NASA OSS ($488k; ranked “outstanding”, not selected due to budget constraints) 2010 PI, “Constraining the Chemical Self-Enrichment of Young Planetary Systems in the Nearest Star-Forming Complex”, NASA OSS ($317k; not selected) 2009 PI, “Improving Age Estimates for Extrasolar Planetary Systems”, NASA OSS ($245k; not selected) 2009 PI, Packard Foundation ($875k; among 100 national nominations, but not selected) 2008 PI, “How Did the Nearest OB Association Form?”, NSF AAG ($248k; not selected) References Prof. Dan M. Watson, Professor, Department of Physics & Astronomy, University of Rochester, Rochester, NY 14627-0171, [email protected] Prof. Michael R. Meyer, Professor (Vice Chair, Institute for Astronomy), ETH Zurich, ETH Ho- enggerberg Campus, Physics Dept., HIT J 22.4, CH-8093 Zurich, Switzerland, +41(0)44-663-4450, [email protected] (Ph.D. advisor) Prof. Lynne Hillenbrand, Professor of Astronomy (Executive Officer), Cahill Center for Astronomy & Astrophysics, California Institute of Technology, MC 249-17, Pasadena, CA 91105, (626) 395-6587, [email protected] Languages English (native), Spanish (advanced) Teaching 2011 spr. AST 241, Stellar Astrophysics (for Jr./Sr.-level majors), UR 2010 fall AST 565, Stellar Astrophysics (graduate), UR 2010 spr. AST 142, Astrophysics II (for Sophomore-level majors), UR 2009 fall AST 111, The Solar System and Its Origin (for Fr./So.-level majors), UR 2009 spr. AST 241, Stellar Astrophysics (for Jr./Sr.-level majors), UR Current Students and Postdocs Advised 2012 Melissa Butner, REU student @ CTIO (spectroscopy) 2011- Duy Nguyen, postdoc (spectroscopy of young stars) 2011- Erin Scott, PhD student (circumstellar disk modeling) 2009- Mark Pecaut, PhD student (star formation history of Sco-Cen) 2009- Scott Barenfeld, UR Class of 2012 (solar wind and coronal X-ray emission) 2008- Marek Slipski, UR Class of 2011 (ages of exoplanet host stars) Past Students and Postdocs Advised 2010-2011 Fred Moolekamp, PhD student (eclipse modeling) 2010 Matt Bourque, REU student/Florida Tech (metallicity of Sco-Cen) 2010 Dilyana Mihaylova, UR Class of 2013 (spectral classification) 2009-2011 Eric Bubar, postdoc (chemical abundances of nearby young stars) 2009-2010 Julieta Gruszko, UR Class of 2012 (REU; activity and ages of Sun-like stars) 2009-2010 Alex Shvonski, PhD student (Spitzer IR survey of debris disks in 32 Ori) Service & Committees (Institutional) (active in bold) 2011- Blanco 4-m Telescope Scientist, CTIO 2011- Hydra Multi-object Spectrograph, Deputy Support Scientist, CTIO 2011- CTIO Website Committee, CTIO 2011 REU/PIA Selection Committee, CTIO 2011 ASNY Spring 2011 Meeting, UR, Local Organizing Committee, Co-chair 2011 UR Physics & Astronomy Colloquium Chair 2011 Qualifying Exam Committee for grad student Mark Pecaut 2010-2011 UR Physics & Astronomy Undergraduate Physics Awards Committee (UAC) 2010-2011 UR Physics & Astronomy Undergraduate Curriculum Committee (UCC) 2010 UR Physics & Astronomy Colloquium Co-chair (w/ J. Eberly) 2010 Qualifying Exam Committee for grad student Kiwan Park 2010 Qualifying Exam Committee for grad student Justin Comparetta 2009-2011 UR Physics & Astronomy Undergraduate Astronomy Advisor 2009-2011 UR Representative to New York Astronomical Corporation 2009-2010 UR Astronomy Group Seminar Chair 2009 Ph.D. Defense Committee for grad student Joel Green 2009 Qualifying Exam Committee for grad student Kyoung Hee Kim 2008-2009 UR Astronomy Group Seminar Co-chair (w/ A. Quillen) Service & Committees (External) (active in bold) 2012 SessionChair-CoolDwarfs,BrownDwarfs- 219th AAS meeting 2010 Judge for Chambliss Astronomy Student Award - 215th AAS meeting 2010 Spitzer Space Telescope Cycle-7, Time Allocation Committee 2008-2009 258th IAU Symposium (The Ages of Stars), proceedings lead editor 2008 Gemini Telescope Time Allocation Committee, external reviewer 2008 Hubble Space Telescope Cycle-17, Time Allocation Committee 2007-2011 NASA Star and Exoplanet Database (NStED), User Panel 2007 Spitzer Space Telescope Cycle-4, Time Allocation Committee 2006 Convener, “Ages of Stars” Splinter Session, Cool Stars 14 meeting 2006-2007 NASA Origins of Solar Systems, external reviewer 2005-2006 Star & Planet Formation Journal Club, organizer (CfA) 2003 Graduate Admissions Committee, Astronomy Dept., UA 2001- Journal Referee: ApJ, AJ, A&A, MNRAS 2001-2003 MIRAC (Mid-Infrared Array Camera) team, observer support at Magellan Professional Memberships American Astronomical Society (AAS) Society of Physics Students (SPS) The Meteoritical Society Sigma Pi Sigma Physics Honor Society (ΣΠΣ) Sigma Xi Scientific Research Society (ΣΞ) International Astronomical Union: Commission 37: Star Clusters and Associations Division VII: Galactic System Division III Commission 53: Extrasolar Planets (WGESP) Invited Talks (past 5 years only) 6/2011 CTIO/Gemini colloquium - La Serena, Chile The Nearest Youngest Stars: Planet Formation Theatre 2/2011 Université de Montréal - Département de Physique - astrophysics colloquium - Montreal What Can Nearby Young Stars Tell Us About Star and Planet Formation? 10/2010In the Spirit of Lyot 2010 - Paris - Ages of Host Stars with Substellar Companions 8/2010 Cool Stars 16 - Juvenile Ultracool Dwarfs Splinter Session - Seattle, WA The Nearby Young Stellar Groups: Demographics and Considerations for Assigning Memberships 1/2010 Pontifica Universidad Catolica de Chile, Astro. Dept. colloquium - Santiago, Chile 9/2009 Stony Brook University Astronomy seminar - Stony Brook, NY 3/2009 Penn State University Astronomy colloquium - State College, PA What Can Nearby Young Stars Tell Us About Star and Planet Formation? 3/2009 2nd Subaru International Conference, Exoplanets and Disks: Their Formation and Diversity - invited review - Keauhou, HI Structure and Evolution of Circumstellar Disks Around Young Stars 10/2008IAU Symposium 258 invited talk - Baltimore, MD The Evolution of Activity Among Solar-Type Stars 3/2008 Northern Arizona University Phys. & Astro. Dept. colloquium - Flagstaff, AZ 2/2008 Georgia State University Phys. & Astro. Dept. colloquium - Atlanta, GA 2/2008 Wesleyan University Astronomy Dept. colloquium - Middletown, CT 2/2008 Gemini South colloquium - La Serena, Chile 1/2008 Space Telescope Science Institute colloquium - Baltimore, MD 11/2007 University of Rochester Physics and Astronomy colloquium - Rochester, USA Where to Study Planet Formation? The Nearest, Youngest Stars 10/2007 Frank N. Bash Symposium 2007: New Horizons in Astronomy Exoplanets and Young
Load more

Recommended publications
  • FY08 Technical Papers by GSMTPO Staff
    AURA/NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation July 23, 2008 Revised as Complete and Submitted December 23, 2008 NGC 660, ~13 Mpc from the Earth, is a peculiar, polar ring galaxy that resulted from two galaxies colliding. It consists of a nearly edge-on disk and a strongly warped outer disk. Image Credit: T.A. Rector/University of Alaska, Anchorage NATIONAL OPTICAL ASTRONOMY OBSERVATORY NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation December 23, 2008 TABLE OF CONTENTS EXECUTIVE SUMMARY ............................................................................................................................. 1 1 SCIENTIFIC ACTIVITIES AND FINDINGS ..................................................................................... 2 1.1 Cerro Tololo Inter-American Observatory...................................................................................... 2 The Once and Future Supernova η Carinae...................................................................................................... 2 A Stellar Merger and a Missing White Dwarf.................................................................................................. 3 Imaging the COSMOS...................................................................................................................................... 3 The Hubble Constant from a Gravitational Lens.............................................................................................. 4 A New Dwarf Nova in the Period Gap............................................................................................................
    [Show full text]
  • Characterisation of Young Nearby Stars – the Ursa Major Group
    FRIEDRICH-SCHILLER-UNIVERSITAT¨ JENA Physikalisch-Astronomische Fakult¨at Characterisation of young nearby stars – The Ursa Major group Dissertation zur Erlangung des akademischen Grades doctor rerum naturalium (Dr. rer. nat.) vorgelegt dem Rat der Physikalischen-Astronomischen Fakult¨at der Friedrich-Schiller-Universit¨at Jena von Dipl.-Phys. Matthias Ammler geboren am 10.01.1977 in Neuburg a. d. Donau Gutachter 1. Prof. Dr. Ralph Neuh¨auser 2. Dr. habil. Matthias H¨unsch 3. Prof. Dr. Artie P. Hatzes Tag der letzten Rigorosumspr¨ufung: 26. Juni 2006 Tag der ¨offentlichen Verteidigung: 11. Juli 2006 Meinen Eltern Contents List of Figures vii List of Tables ix Abstract xi Zusammenfassung xiii Remarks and Acknowledgements xv 1 Introduction 1 1.1 WhatistheUrsaMajorgroup? . 1 1.1.1 Co-movingstarsin the BigDipper constellation . .... 1 1.1.2 Stellarmotionandmovinggroups . 1 1.1.3 Formation and evolution of open clusters and associations ... 6 1.1.4 The nature of the UMa group – cluster or association, or some- thingelse? ............................ 8 1.2 WhyistheUMagroupinteresting?. 8 1.2.1 Asnapshotinstellarevolution . 8 1.2.2 Alaboratoryinfrontofthedoor . 9 1.2.3 Thecensusofthesolarneighbourhood . 10 1.3 ConstrainingtheUMagroup–previousapproaches . ..... 11 1.3.1 Spatialclustering . 11 1.3.2 Kinematic criteria – derived from a “canonical” memberlist . 12 1.3.3 Kinematic parameters – derived from kinematic clustering ... 15 1.3.4 Stellarparametersandabundances . 17 1.3.5 TheageoftheUMagroup–photometriccriteria . 19 1.3.6 Spectroscopicindicatorsforageandactivity . .... 19 1.3.7 Combining kinematic, spectroscopic, and photometric criteria . 21 1.4 Anewhomogeneousspectroscopicstudy . 21 1.4.1 Definingthesample ....................... 22 1.4.2 Howtoobtainprecisestellarparameters? . .. 23 2 Observations,reductionandcalibration 25 2.1 Requireddata ............................... 25 2.2 Instruments ...............................
    [Show full text]
  • Young Nearby Stars by Adam Conrad Schneider (Under The
    Young Nearby Stars by Adam Conrad Schneider (Under the Direction of Professor Inseok Song) Abstract Nearby young stars are without equal as stellar and planetary evolution laboratories. The aim of this work is to use age diagnostic considerations to execute a complete survey for new nearby young stars and to efficiently reevaluate and constrain their ages. Because of their proximity and age, young, nearby stars are the most desired targets for any astrophysical study focusing on the early stages of star and planet formation. Identifying nearby, young, low-mass stars is challenging because of their inherent faint- ness and age diagnostic degeneracies. A new method for identifying these objects has been developed, and a pilot study of its effectiveness is demonstrated by the identification of two definite new members of the TW Hydrae Association. Nearby, young, solar-type stars are initially identified in this work by their fractional X-ray luminosity. The results of a large-scale search for nearby, young, solar-type stars is presented. Follow-up spectroscopic observations are taken in order to measure various age diagnostics in order to accurately assess stellar ages. Age, one of the most fundamental properties of a star, is also one of the most difficult to determine. While a variety of proce- dures have been developed and utilized to approximate ages for solar-type stars, with varying degrees of success, a comprehensive age-dating technique has yet to be constructed. Often- times, different methods exhibit contradictory or conflicting findings. Such inconsistencies demonstrate the value of a uniform method of determining stellar ages.
    [Show full text]
  • Curriculum Vitae - 24 March 2020
    Dr. Eric E. Mamajek Curriculum Vitae - 24 March 2020 Jet Propulsion Laboratory Phone: (818) 354-2153 4800 Oak Grove Drive FAX: (818) 393-4950 MS 321-162 [email protected] Pasadena, CA 91109-8099 https://science.jpl.nasa.gov/people/Mamajek/ Positions 2020- Discipline Program Manager - Exoplanets, Astro. & Physics Directorate, JPL/Caltech 2016- Deputy Program Chief Scientist, NASA Exoplanet Exploration Program, JPL/Caltech 2017- Professor of Physics & Astronomy (Research), University of Rochester 2016-2017 Visiting Professor, Physics & Astronomy, University of Rochester 2016 Professor, Physics & Astronomy, University of Rochester 2013-2016 Associate Professor, Physics & Astronomy, University of Rochester 2011-2012 Associate Astronomer, NOAO, Cerro Tololo Inter-American Observatory 2008-2013 Assistant Professor, Physics & Astronomy, University of Rochester (on leave 2011-2012) 2004-2008 Clay Postdoctoral Fellow, Harvard-Smithsonian Center for Astrophysics 2000-2004 Graduate Research Assistant, University of Arizona, Astronomy 1999-2000 Graduate Teaching Assistant, University of Arizona, Astronomy 1998-1999 J. William Fulbright Fellow, Australia, ADFA/UNSW School of Physics Languages English (native), Spanish (advanced) Education 2004 Ph.D. The University of Arizona, Astronomy 2001 M.S. The University of Arizona, Astronomy 2000 M.Sc. The University of New South Wales, ADFA, Physics 1998 B.S. The Pennsylvania State University, Astronomy & Astrophysics, Physics 1993 H.S. Bethel Park High School Research Interests Formation and Evolution
    [Show full text]
  • Winter Observing Notes
    Wynyard Planetarium & Observatory Winter Observing Notes Wynyard Planetarium & Observatory PUBLIC OBSERVING – Winter Tour of the Sky with the Naked Eye NGC 457 CASSIOPEIA eta Cas Look for Notice how the constellations 5 the ‘W’ swing around Polaris during shape the night Is Dubhe yellowish compared 2 Polaris to Merak? Dubhe 3 Merak URSA MINOR Kochab 1 Is Kochab orange Pherkad compared to Polaris? THE PLOUGH 4 Mizar Alcor Figure 1: Sketch of the northern sky in winter. North 1. On leaving the planetarium, turn around and look northwards over the roof of the building. To your right is a group of stars like the outline of a saucepan standing up on it’s handle. This is the Plough (also called the Big Dipper) and is part of the constellation Ursa Major, the Great Bear. The top two stars are called the Pointers. Check with binoculars. Not all stars are white. The colour shows that Dubhe is cooler than Merak in the same way that red-hot is cooler than white-hot. 2. Use the Pointers to guide you to the left, to the next bright star. This is Polaris, the Pole (or North) Star. Note that it is not the brightest star in the sky, a common misconception. Below and to the right are two prominent but fainter stars. These are Kochab and Pherkad, the Guardians of the Pole. Look carefully and you will notice that Kochab is slightly orange when compared to Polaris. Check with binoculars. © Rob Peeling, CaDAS, 2007 version 2.0 Wynyard Planetarium & Observatory PUBLIC OBSERVING – Winter Polaris, Kochab and Pherkad mark the constellation Ursa Minor, the Little Bear.
    [Show full text]
  • Constellation Studies - Equatorial Sky in Winter
    Phys1810: General Astronomy 1 W2014 Constellation Studies - Equatorial Sky in Winter Preparation before the observing session - Read "Notes on Observing" thoroughly. - Find all the targets listed below using Starry Night and your star charts. - Note: The observatory longitude is 97.1234° W, the latitude is 49.6452° N and elevation is 233 meters. - Observe any predicted events and record your observations during the observing session In the list of constellations below, the name of the constellation is underlined followed by the genitive case of the name in parenthesis followed by the three-letter abbreviation. Note that references to stars such as α UMa, spoken as alpha Ursae Majoris (note genitive case), literally means alpha of Ursa Major. The Greek letters are usually assigned in order of brightness in the constellation (α -- brightest). Note that the constellation, Ursa Major, is a major exception to this rule. As soon as you get to the observatory the following 3 constellations should be sketched on a full page diagram making sure that their relative positions to each other and to the horizon are drawn as accurately as possible - this means completing the sketch in about 15 minutes. You need to repeat the sketch one hour later. Be sure to indicate the time and the location of the horizon on your diagram. Ursa Major (Ursae Majoris) UMa: (The Great Bear, The Big Dipper, The Plow) Through all ages, Ursa Major has been known under various names. It is linked with the nymph Kallisto, the daughter of Lycaon, a king of Arcadia in Greek mythology. Moving along the asterism of the dipper from the lip identify the stars Dubhe (α UMa), Merak (β UMa), Phecda (γ UMa), Megrez (δ UMa), Alioth (ε UMa), Mizar (ζ UMa), and Alkaid (η UMa).
    [Show full text]
  • Focus on Zeta Ursae Majoris - Mizar
    Vol. 3 No. 2 Spring 2007 Journal of Double Star Observations Page 51 Stargazers Corner: Focus on Zeta Ursae Majoris - Mizar Jim Daley Ludwig Schupmann Observatory (LSO) New Ipswich, New Hampshire Email: [email protected] Abstract: : This is a general interest article for both the double star viewer and armchair astronomer alike. By highlighting an interesting pair, hopefully in each issue, we have a place for those who love doubles but may have little interest in the rigors of measurements and the long lists of results. Your comments about these mini-articles are welcomed. Arabs long ago named Alcor “Saidak” or “the proof” as Introduction they too used it as a test of vision. Alcor shares nearly My first view of a double star through a telescope the same space motion with Mizar and about 20 other was an inspiring sight and just as with many new stars in what is called the Ursa Major stream or observers today, the star was Mizar. As a beginning moving cluster. The Big Dipper is considered the amateur telescope maker (1951) I followed tradition closest cluster in the solar neighborhood. Alcor’s and began to use closer doubles for resolution testing apparent separation from Mizar is more than a quar- the latest homemade instrument. Visualizing the ter light year and this alone just about rules out this scale of binaries, their physical separation, Keplerian wide pair from being a physical (in a binary star motion, orbital period, component diameters and sense) system and the most recent line-of-sight dis- spectral characteristics, all things I had heard and tance measurements give a difference between them read of, seemed a bit complicated at the time and, I of about 3 light years, ending any ideas of an orbiting might add, more so now! Through the years I found pair.
    [Show full text]
  • The Twofold Debris Disk Around HD 113766 A⋆
    A&A 551, A134 (2013) Astronomy DOI: 10.1051/0004-6361/201220904 & c ESO 2013 Astrophysics The twofold debris disk around HD 113766 A? Warm and cold dust as seen with VLTI/MIDI and Herschel/PACS J. Olofsson1, Th. Henning1, M. Nielbock1, J.-C. Augereau2, A. Juhàsz3, I. Oliveira4, O. Absil5, and A. Tamanai6 1 Max Planck Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany e-mail: [email protected] 2 UJF-Grenoble 1/CNRS-INSU, Institut de Planétologie et d’Astrophysique de Grenoble (IPAG), UMR 5274, Grenoble, France 3 Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands 4 Astronomy Department, University of Texas at Austin, 1 University Station C1400, Austin, TX 78712-0259, USA 5 Département d’Astrophysique, Géophysique et Océanographie, Université de Liège, 17 Allée du Six Août, 4000 Sart Tilman, Belgium 6 University Heidelberg, Kirchhoff-Institut für Physik, 69120 Heidelberg, Germany Received 13 December 2012 / Accepted 22 January 2013 ABSTRACT Context. Warm debris disks are a sub-sample of the large population of debris disks, and display excess emission in the mid-infrared. Around solar-type stars, very few objects (∼2% of all debris disks) show emission features in mid-IR spectroscopic observations that are attributed to small, warm silicate dust grains. The origin of this warm dust could be explained either by a recent catastrophic collision between several bodies or by transport from an outer belt similar to the Kuiper belt in the solar system. Aims. We present and analyze new far-IR Herschel/PACS photometric observations, supplemented by new and archival ground-based data in the mid-IR (VLTI/MIDI and VLT/VISIR), for one of these rare systems: the 10–16 Myr old debris disk around HD 113766 A.
    [Show full text]
  • Astro-Ph 2006第2週
    2020年 6月 第2週 新着論文サーベイ 6 月 8 日 (月曜日) [1] arxive:2006.03120 Title: ”Dual-Wavelength ALMA Observations of Dust Rings in Protoplanetary Disks” Author:Feng Long, Paola Pinilla, Gregory J. Herczeg, Sean M. Andrews, Daniel Harsono, Doug Johnstone, Enrico Ragusa, Ilaria Pascucci, David J. Wilner, Nathan Hendler, Jeff Jennings, Yao Liu, Giuseppe Lodato, Francois Menard, Gerrit van de Plas, Giovanni Dipierro Comments: accepted for publication in ApJ Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Astrophysics of Galaxies (astro-ph.GA); Solar and Stellar Astrophysics (astro-ph.SR) [観測/ALMA] 原始惑星系円盤中にリング状の構造を持つDS Tau, GO Tau, DL Tau を 、ALMA で 観 測 し た 。波 長1.3 は mm と 2.9 mm の 2 バ ン ド で 、角 分 解 能 は と も0.1 に秒 角 。2 バ ン ド で リ ン グ の 端 の 位 置 は 同 じ で あ っ た 。こ の こ と を 、ダ ス ト 進化のモデルで説明した。 [2] arxive:2006.03113 Title: ”The size, shape, density and ring of the dwarf planet Haumea from a stellar occultation” Author:J. L. Ortiz, P. Santos-Sanz, B. Sicardy, G. Benedetti-Rossi, D. Bérard, N. Morales, R. Duffard, F. Braga-Ribas, U. Hopp, C. Ries, V. Nascim- beni, F. Marzari, V. Granata, A. Pál, C. Kiss, T. Pribulla, R. Komžík, K. Hornoch, P. Pravec, P. Bacci, M. Maestripieri, L. Nerli, L. Mazzei, M. Bachini, F. Martinelli, G. Succi, F. Ciabattari, H. Mikuz, A. Carbog- nani, B. Gaehrken, S. Mottola, S. Hellmic, F. L. Rommel, E. Fernández- Valenzuela, A. Campo Bagatin, S. Cikota, A.
    [Show full text]
  • The Observer's Handbook for 1915
    T he O b s e r v e r ’s H a n d b o o k FOR 1915 PUBLISHED BY The Royal Astronomical Society Of Canada E d i t e d b y C . A. CHANT SEVENTH YEAR OF PUBLICATION TORONTO 198 C o l l e g e S t r e e t Pr in t e d f o r t h e S o c ie t y CALENDAR 1915 T he O bserver' s H andbook FOR 1915 PUBLISHED BY The Royal Astronomical Society Of Canada E d i t e d b y C. A. CHANT SEVENTH YEAR OF PUBLICATION TORONTO 198 C o l l e g e S t r e e t Pr in t e d f o r t h e S o c ie t y 1915 CONTENTS Preface - - - - - - 3 Anniversaries and Festivals - - - - - 3 Symbols and Abbreviations - - - - -4 Solar and Sidereal Time - - - - 5 Ephemeris of the Sun - - - - 6 Occultation of Fixed Stars by the Moon - - 8 Times of Sunrise and Sunset - - - - 8 The Sky and Astronomical Phenomena for each Month - 22 Eclipses, etc., of Jupiter’s Satellites - - - - 46 Ephemeris for Physical Observations of the Sun - - 48 Meteors and Shooting Stars - - - - - 50 Elements of the Solar System - - - - 51 Satellites of the Solar System - - - - 52 Eclipses of Sun and Moon in 1915 - - - - 53 List of Double Stars - - - - - 53 List of Variable Stars- - - - - - 55 The Stars, their Magnitude, Velocity, etc. - - - 56 The Constellations - - - - - - 64 Comets of 1914 - - - - - 76 PREFACE The H a n d b o o k for 1915 differs from that for last year chiefly in the omission of the brief review of astronomical pro­ gress, and the addition of (1) a table of double stars, (2) a table of variable stars, and (3) a table containing 272 stars and 5 nebulae.
    [Show full text]
  • Age Dating the Galactic Bar with the Nuclear Stellar Disc
    MNRAS 492, 4500–4511 (2020) doi:10.1093/mnras/staa140 Advance Access publication 2020 January 20 Age dating the Galactic bar with the nuclear stellar disc Downloaded from https://academic.oup.com/mnras/article-abstract/492/3/4500/5709929 by Institute of Child Health/University College London user on 14 February 2020 Junichi Baba1‹ and Daisuke Kawata 2 1National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan 2Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, UK Accepted 2020 January 11. Received 2019 December 26; in original form 2019 September 16 ABSTRACT From the decades of the theoretical studies, it is well known that the formation of the bar triggers the gas funnelling into the central sub-kpc region and leads to the formation of a kinematically cold nuclear stellar disc (NSD). We demonstrate that this mechanism can be used to identify the formation epoch of the Galactic bar, using an N-body/hydrodynamics simulation of an isolated Milky Way–like galaxy. As shown in many previous literature, our simulation shows that the bar formation triggers an intense star formation for ∼1 Gyr in the central region and forms an NSD. As a result, the oldest age limit of the NSD is relatively sharp, and the oldest population becomes similar to the age of the bar. Therefore, the age distribution of the NSD tells us the formation epoch of the bar. We discuss that a major challenge in measuring the age distribution of the NSD in the Milky Way is contamination from other non-negligible stellar components in the central region, such as a classical bulge component.
    [Show full text]
  • Ages of Young Stars
    Ages of Young Stars David R. Soderblom Space Telescope Science Institute, Baltimore MD USA Lynne A. Hillenbrand Caltech, Pasadena CA USA Rob. D. Jeffries Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK Eric E. Mamajek Department of Physics & Astronomy, University of Rochester, Rochester NY, 14627-0171, USA Tim Naylor School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL, UK Determining the sequence of events in the formation of stars and planetary systems and their time-scales is essential for understanding those processes, yet establishing ages is fundamentally difficult because we lack direct indicators. In this review we discuss the age challenge for young stars, specifically those less than ∼100 Myr old. Most age determination methods that we discuss are primarily applicable to groups of stars but can be used to estimate the age of individual objects. A reliable age scale is established above 20 Myr from measurement of the Lithium Depletion Boundary (LDB) in young clusters, and consistency is shown between these ages and those from the upper main sequence and the main sequence turn-off – if modest core convection and rotation is included in the models of higher-mass stars. Other available methods for age estimation include the kinematics of young groups, placing stars in Hertzsprung-Russell diagrams, pulsations and seismology, surface gravity measurement, rotation and activity, and lithium abundance. We review each of these methods and present known strengths and weaknesses. Below ∼ 20 Myr, both model-dependent and observational uncertainties grow, the situation is confused by the possibility of age spreads, and no reliable absolute ages yet exist.
    [Show full text]