DOCSLIB.ORG

Planets in Binary Systems: Studies with Precise Radial Velocities and High-Resolution Imaging

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Planets in Binary Systems: Studies with Precise Radial Velocities and High-Resolution Imaging Planets in Binary Systems: Studies with Precise Radial Velocities and High-Resolution Imaging By Lea Hirsch A dissertation submitted in partial satisfaction of the requirements for the degree of Doctor of Philosophy in Astrophysics in the Graduate Division of the University of California, Berkeley Committee in charge: Professor James Graham, Chair Professor Eugene Chiang Professor Burkhard Militzer Summer 2018 Planets in Binary Systems: Studies with Precise Radial Velocities and High-Resolution Imaging Copyright 2018 by Lea Hirsch 1 Abstract Planets in Binary Systems: Studies with Precise Radial Velocities and High-Resolution Imaging by Lea Hirsch Doctor of Philosophy in Astrophysics University of California, Berkeley Professor James Graham, Chair Nearly half of all solar-type stars have at least one stellar or brown dwarf companion, and planets around G- and K-type stars appear to be quite common. Yet the impact of stellar multiplicity on planets, and on our understanding of planets, is not well understood. In this thesis, I describe a combination of work to study the interplay between stellar and planetary companions, using the combination of radial velocity and high-resolution imaging observations. First, planets discovered by transit surveys like the Kepler Mission are sensitive to a detection and characterization bias due to stellar companions. The light of unresolved binary companions dilutes the transit of the planet, making it appear shallower than it is. This causes planet sizes in binary systems to be underestimated, and sensitivity to small planets to be overestimated. In Chapter2, I combined multi-wavelength observations of stellar companions detected within 200of 170 Kepler Object of Interest hosts, to assess whether these companions were physically associated with the planet host stars. I found that stellar companions within 100 had a ≥ 80% likelihood of being bound. I used the compiled imaging observations of the bound stellar companions in this sample to determine the factor by which planet radii in these systems were underestimated. I determined that an average radius correction factor of XR = 1:65 must be applied to planets orbiting stars with unresolved stellar companions, assuming the planets are equally likely to orbit either of the stars in a binary system. This means that planets in unresolved binary systems may have radii underestimated by an average of 65%. This effect is particularly important for Kepler stars with minimal ground-based follow-up; by performing a combination of spectroscopic and imaging observations on Kepler planet hosts, it is possible to reduce the effect of stellar companions by finding or ruling out binary companions in large regions of parameter space. Second, stellar companions likely impact the formation and evolution of planetary sys- tems. To probe these effects, I focused on the solar neighborhood, studying sun-like stars within 25 pc using Doppler spectroscopy as well as adaptive optics and speckle imaging 2 techniques. I built up methodology for performing joint orbital fits to combinations of radial velocity, astrometric, and photometric data by assessing the orbit of HD 159062in Chapter3. HD 159062 is a nearby binary system consisting of a G dwarf and a newly-discovered white +0:09 dwarf companion. I determined that the white dwarf must have a mass of 0:54−0:03M . Its combined radial velocities, astrometry, and photometry are inconsistent with it being either a brown dwarf or a main sequence star. In Chapter4, I extended this joint orbital analysis technique to make use of imaging non-detections to place constraints on orbiting planets. In this study, we focused on the nearby adolescent K dwarf, Eridani, whose giant planet was detected in three decades of radial velocity monitoring. Using deep M-band coronographic imaging that resulted in no detection of the planet, upper limits were placed on the mass of the giant planet. The combination of the RV data and constraints from the non-detection of the planet allowed the mass and inclination of the planet to be determined more precisely than with the RV data alone. Finally, I performed a simultaneous RV and imaging survey for both stellar and planetary companions to sun-like stars in the solar neighborhood in Chapter5. By comparing the planet occurrence rates in binary systems to those in single star systems, we can begin to untangle the effects of stellar companions on planet formation. I found that the occurrence rate of planets with masses between 0.1 and 10 MJand with semi-major axes between 0.1 and 10 AU is statistically equivalent in single star and binary star systems. I also determined that all known planet-hosting binary systems in the 25 pc sun-like star sample had separations wider than 100 AU. This indicates that wide binary companions do not seem to strongly impact the planet formation process, but that the planet occurrence rate in binary systems may decrease for systems with smaller binary separations. i To Miriam and Howard Hirsch ii Contents List of Figuresv List of Tables vii Acknowledgments viii 1 Introduction1 1.1 Stellar Multiplicity................................1 1.1.1 Multiplicity in the Solar Neighborhood.................1 1.2 The Effects of Stellar Companions on Planets.................2 1.2.1 Theories of Exoplanet Formation and Evolution............2 1.2.2 Previous Observational Constraints...................4 1.2.3 Characterization of Transiting Planets.................5 1.3 Combining Radial Velocities and Imaging....................6 1.4 This Thesis....................................7 2 Assessing the Effect of Stellar Companions from High-Resolution Imaging of Kepler Objects of Interest 10 2.1 Introduction.................................... 10 2.2 Sample....................................... 12 2.2.1 KOI Host Stars.............................. 12 2.2.2 Stellar Companions............................ 15 2.3 Determining Physical Association of Companion Stars............. 16 2.3.1 Interstellar Extinction.......................... 21 2.3.2 Comparison with Stellar Population Models.............. 22 2.4 Bound Companions to Kepler Planet Hosts................... 23 2.5 Planet Radius Corrections............................ 28 2.6 Conclusions.................................... 35 3 Combining Radial Velocities and Direct Imaging to Constrain the Orbit of the White Dwarf Companion to HD 159062 38 3.1 Introduction.................................... 38 3.2 Observations and Data Reduction........................ 41 Contents iii 3.2.1 Radial Velocity Observations....................... 41 3.2.2 High-Resolution Imaging......................... 41 3.3 Astrometry and Common Proper Motion.................... 46 3.4 HD 159062 B is not a Brown Dwarf....................... 46 3.5 Orbital Analysis.................................. 48 3.5.1 White Dwarf Cooling Models...................... 50 3.5.2 Total system age............................. 52 3.6 Discussion..................................... 55 3.7 Conclusions.................................... 55 4 Deep exploration of Eridani with Keck Ms-band vortex coronagraphy and radial velocities: mass and orbital parameters of the giant exoplanet 57 4.1 Introduction.................................... 57 4.1.1 Eridani’s debris disk.......................... 57 4.1.2 Eridani’s putative planet........................ 59 4.1.3 This chapter................................ 59 4.2 Doppler Spectroscopy............................... 60 4.2.1 RV observations.............................. 60 4.2.2 RV data analysis............................. 61 4.3 High contrast imaging.............................. 62 4.3.1 High contrast imaging observations................... 62 4.3.2 Image post-processing.......................... 63 4.4 Results....................................... 63 4.4.1 Robust detection limits from direct imaging.............. 63 4.4.2 Tests on the RV Data.......................... 68 4.4.3 Combining constraints from imaging and RV.............. 75 4.5 Discussion..................................... 78 4.5.1 Choice of evolutionary models...................... 81 4.5.2 Constraints on the system’s age and inclination............ 82 4.5.3 Planet-disk interactions......................... 85 4.6 Conclusion..................................... 89 5 Understanding the Impacts of Stellar Companions on Planet Formation and Evolution: A Survey of Stellar and Planetary Companions within 25 pc 97 5.1 Introduction.................................... 97 5.2 25 pc Sample................................... 99 5.3 High-Resolution Imaging Observations..................... 99 5.3.1 Lick/ShaneAO.............................. 100 5.3.2 Palomar/PHARO............................. 104 5.4 Radial Velocity Observations........................... 104 5.4.1 Keck/HIRES............................... 105 Contents iv 5.4.2 APF/Levy................................. 106 5.5 Stellar Companions................................ 106 5.5.1 Sensitivity to Stellar Companions.................... 111 5.6 Planetary Companions.............................. 115 5.6.1 Blind Planet Search............................ 115 5.6.2 New Planet Detections.......................... 120 5.6.3 Sensitivity to Planets........................... 122 5.7 Planet Occurrence in Single and Binary Systems............... 127 5.8 Discussion..................................... 132 5.9 Conclusions.................................... 134 Bibliography 135 v List of Figures 2.1 Kepler magnitudes for sample KOI host stars..................
Load more

Recommended publications
  • Summer Constellations
    Night Sky 101: Summer Constellations The Summer Triangle Photo Credit: Smoky Mountain Astronomical Society The Summer Triangle is made up of three bright stars—Altair, in the constellation Aquila (the eagle), Deneb in Cygnus (the swan), and Vega Lyra (the lyre, or harp). Also called “The Northern Cross” or “The Backbone of the Milky Way,” Cygnus is a horizontal cross of five bright stars. In very dark skies, Cygnus helps viewers find the Milky Way. Albireo, the last star in Cygnus’s tail, is actually made up of two stars (a binary star). The separate stars can be seen with a 30 power telescope. The Ring Nebula, part of the constellation Lyra, can also be seen with this magnification. In Japanese mythology, Vega, the celestial princess and goddess, fell in love Altair. Her father did not approve of Altair, since he was a mortal. They were forbidden from seeing each other. The two lovers were placed in the sky, where they were separated by the Celestial River, repre- sented by the Milky Way. According to the legend, once a year, a bridge of magpies form, rep- resented by Cygnus, to reunite the lovers. Photo credit: Unknown Scorpius Also called Scorpio, Scorpius is one of the 12 Zodiac constellations, which are used in reading horoscopes. Scorpius represents those born during October 23 to November 21. Scorpio is easy to spot in the summer sky. It is made up of a long string bright stars, which are visible in most lights, especially Antares, because of its distinctly red color. Antares is about 850 times bigger than our sun and is a red giant.
    [Show full text]
  • September 2016
    11/20/2016 11:13 AM CHECK RECONCILIATION REGISTER PAGE: 1 COMPANY: 04 - COMMUNITY DEVELOPMENT CHECK DATE: 9/01/2016 THRU 9/30/2016 ACCOUNT: 10010 CASH C.D.B.G. - CHECKING CLEAR DATE: 0/00/0000 THRU 99/99/9999 TYPE: Check STATEMENT: 0/00/0000 THRU 99/99/9999 STATUS: All VOIDED DATE: 0/00/0000 THRU 99/99/9999 FOLIO: All AMOUNT: 0.00 THRU 999,999,999.99 CHECK NUMBER: 000000 THRU 999999 ACCOUNT --DATE-- --TYPE-- NUMBER ---------DESCRIPTION---------- ----AMOUNT--- STATUS FOLIO CLEAR DATE CHECK: ---------------------------------------------------------------------------------------------------------------- 10010 9/08/2016 CHECK 006680 LOWER RIO GRANDE VALLEY 1,702.00CR CLEARED A 10/10/2016 10010 9/08/2016 CHECK 006681 MISSION CRIME STOPPERS 2,726.60CR CLEARED A 10/10/2016 10010 9/22/2016 CHECK 006682 A ONE INSULATION 5,950.00CR CLEARED A 10/10/2016 10010 9/22/2016 CHECK 006683 A ONE INSULATION 5,950.00CR CLEARED A 10/10/2016 10010 9/22/2016 CHECK 006684 A ONE INSULATION 5,850.00CR CLEARED A 10/10/2016 10010 9/22/2016 CHECK 006685 A ONE INSULATION 5,850.00CR CLEARED A 10/10/2016 10010 9/22/2016 CHECK 006686 CHILDREN'S ADV.CENTER HDL 911.62CR CLEARED A 10/10/2016 10010 9/22/2016 CHECK 006687 G&G CONTRACTORS 23,920.00CR CLEARED A 10/10/2016 10010 9/29/2016 CHECK 006688 AMIGOS DEL VALLE 1,631.05CR CLEARED A 11/07/2016 10010 9/29/2016 CHECK 006689 DELL MARKETING L.P. 1,148.00CR CLEARED A 11/07/2016 10010 9/29/2016 CHECK 006690 LOWER RIO GRANDE VALLEY 2,682.54CR CLEARED A 11/07/2016 10010 9/29/2016 CHECK 006691 SILVER RIBBON COMMUNITY PARTNE 815.04CR
    [Show full text]
  • A Large Hα Line Forming Region for the Massive Interacting Binaries Β
    A&A 532, A148 (2011) Astronomy DOI: 10.1051/0004-6361/201116742 & c ESO 2011 Astrophysics AlargeHα line forming region for the massive interacting binaries β Lyrae and υ Sagitarii D. Bonneau1, O. Chesneau1, D. Mourard1, Ph. Bério1,J.M.Clausse1, O. Delaa1,A.Marcotto1, K. Perraut2, A. Roussel1,A.Spang1,Ph.Stee1, I. Tallon-Bosc3, H. McAlister4,5, T. ten Brummelaar5, J. Sturmann5, L. Sturmann5, N. Turner5, C. Farrington5, and P. J. Goldfinger5 1 Lab. H. Fizeau, Univ. Nice Sophia Antipolis, CNRS UMR 6525, Obs. de la Côte d’Azur, Av. Copernic, 06130 Grasse, France e-mail: [email protected] 2 UJF-Grenoble 1/CNRS-INSU, Inst. de Planétologie et d’Astrophysique de Grenoble (IPAG) UMR 5274, Grenoble 38041, France 3 Univ. Lyon 1, Observatoire de Lyon, 9 avenue Charles André, Saint-Genis Laval 69230, France 4 Georgia State University, PO Box 3969, Atlanta GA 30302-3969, USA 5 CHARA Array, Mount Wilson Observatory, 91023 Mount Wilson CA, USA Received 17 February 2011 / Accepted 1 July 2011 ABSTRACT Aims. This study aims at constraining the properties of two interacting binary systems by measuring their continuum-forming region in the visible and the forming regions of some emission lines, in particular Hα, using optical interferometry. Methods. We have obtained visible medium (R ∼ 1000) spectral resolution interferometric observations of β Lyr and of υ Sgr using the VEGA instrument of the CHARA array. For both systems, visible continuum (520/640 nm) visibilities were estimated and differential interferometry data were obtained in the Hα emission line at several epochs of their orbital period.
    [Show full text]
  • Naming the Extrasolar Planets
    Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named.
    [Show full text]
  • Our Place in the Universe Research Earth Orbits the Sun, Slowly Traveling Around in a Circular Path
    Earth, Sun, and Moon System Explore 2 Our Place in the Universe Research Earth orbits the Sun, slowly traveling around in a circular path. The Sun is a middle sized star. All of the planets in our solar system orbit this star. But when you look up at the night sky, you will see many other stars. Some of those have their own planets orbiting away in space. These other solar systems are called exosolar systems to distinguish between our solar system and these alien systems. Almost all of the objects you see in the night sky are part of the Milky Way, which is a giant collection of stars that all orbit a common center due to gravity. But if you look at the constellation Pegasus, which makes a giant square in the summer sky, you might see what appears to be a puffy cloud nearby. It is not a cloud, though. It is the Andromeda galaxy. It is an even bigger collection of stars that orbit a common center, and is over a million light-years away! There are many millions of galaxies in our universe, some close by and others very distant. Your group will choose one of these types of objects (stars, exosolar systems, and galaxies) and research its properties and location in the universe. You will then create a poster and a presentation about your star, galaxy, or exosolar system to present to the class. Procedure: 1. With your group, research one of the following objects. These are not the only options, but simply suggestions.
    [Show full text]
  • The Midnight Sky: Familiar Notes on the Stars and Planets, Edward Durkin, July 15, 1869 a Good Way to Start – Find North
    The expression "dog days" refers to the period from July 3 through Aug. 11 when our brightest night star, SIRIUS (aka the dog star), rises in conjunction* with the sun. Conjunction, in astronomy, is defined as the apparent meeting or passing of two celestial bodies. TAAS Fabulous Fifty A program for those new to astronomy Friday Evening, July 20, 2018, 8:00 pm All TAAS and other new and not so new astronomers are welcome. What is the TAAS Fabulous 50 Program? It is a set of 4 meetings spread across a calendar year in which a beginner to astronomy learns to locate 50 of the most prominent night sky objects visible to the naked eye. These include stars, constellations, asterisms, and Messier objects. Methodology 1. Meeting dates for each season in year 2018 Winter Jan 19 Spring Apr 20 Summer Jul 20 Fall Oct 19 2. Locate the brightest and easiest to observe stars and associated constellations 3. Add new prominent constellations for each season Tonight’s Schedule 8:00 pm – We meet inside for a slide presentation overview of the Summer sky. 8:40 pm – View night sky outside The Midnight Sky: Familiar Notes on the Stars and Planets, Edward Durkin, July 15, 1869 A Good Way to Start – Find North Polaris North Star Polaris is about the 50th brightest star. It appears isolated making it easy to identify. Circumpolar Stars Polaris Horizon Line Albuquerque -- 35° N Circumpolar Stars Capella the Goat Star AS THE WORLD TURNS The Circle of Perpetual Apparition for Albuquerque Deneb 1 URSA MINOR 2 3 2 URSA MAJOR & Vega BIG DIPPER 1 3 Draco 4 Camelopardalis 6 4 Deneb 5 CASSIOPEIA 5 6 Cepheus Capella the Goat Star 2 3 1 Draco Ursa Minor Ursa Major 6 Camelopardalis 4 Cassiopeia 5 Cepheus Clock and Calendar A single map of the stars can show the places of the stars at different hours and months of the year in consequence of the earth’s two primary movements: Daily Clock The rotation of the earth on it's own axis amounts to 360 degrees in 24 hours, or 15 degrees per hour (360/24).
    [Show full text]
  • Arxiv:2105.11583V2 [Astro-Ph.EP] 2 Jul 2021 Keck-HIRES, APF-Levy, and Lick-Hamilton Spectrographs
    Draft version July 6, 2021 Typeset using LATEX twocolumn style in AASTeX63 The California Legacy Survey I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades Lee J. Rosenthal,1 Benjamin J. Fulton,1, 2 Lea A. Hirsch,3 Howard T. Isaacson,4 Andrew W. Howard,1 Cayla M. Dedrick,5, 6 Ilya A. Sherstyuk,1 Sarah C. Blunt,1, 7 Erik A. Petigura,8 Heather A. Knutson,9 Aida Behmard,9, 7 Ashley Chontos,10, 7 Justin R. Crepp,11 Ian J. M. Crossfield,12 Paul A. Dalba,13, 14 Debra A. Fischer,15 Gregory W. Henry,16 Stephen R. Kane,13 Molly Kosiarek,17, 7 Geoffrey W. Marcy,1, 7 Ryan A. Rubenzahl,1, 7 Lauren M. Weiss,10 and Jason T. Wright18, 19, 20 1Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 2IPAC-NASA Exoplanet Science Institute, Pasadena, CA 91125, USA 3Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 4Department of Astronomy, University of California Berkeley, Berkeley, CA 94720, USA 5Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 6Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA 7NSF Graduate Research Fellow 8Department of Physics & Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA 9Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 10Institute for Astronomy, University of Hawai`i,
    [Show full text]
  • Thinking Outside the Sphere Views of the Stars from Aristotle to Herschel Thinking Outside the Sphere
    Thinking Outside the Sphere Views of the Stars from Aristotle to Herschel Thinking Outside the Sphere A Constellation of Rare Books from the History of Science Collection The exhibition was made possible by generous support from Mr. & Mrs. James B. Hebenstreit and Mrs. Lathrop M. Gates. CATALOG OF THE EXHIBITION Linda Hall Library Linda Hall Library of Science, Engineering and Technology Cynthia J. Rogers, Curator 5109 Cherry Street Kansas City MO 64110 1 Thinking Outside the Sphere is held in copyright by the Linda Hall Library, 2010, and any reproduction of text or images requires permission. The Linda Hall Library is an independently funded library devoted to science, engineering and technology which is used extensively by The exhibition opened at the Linda Hall Library April 22 and closed companies, academic institutions and individuals throughout the world. September 18, 2010. The Library was established by the wills of Herbert and Linda Hall and opened in 1946. It is located on a 14 acre arboretum in Kansas City, Missouri, the site of the former home of Herbert and Linda Hall. Sources of images on preliminary pages: Page 1, cover left: Peter Apian. Cosmographia, 1550. We invite you to visit the Library or our website at www.lindahlll.org. Page 1, right: Camille Flammarion. L'atmosphère météorologie populaire, 1888. Page 3, Table of contents: Leonhard Euler. Theoria motuum planetarum et cometarum, 1744. 2 Table of Contents Introduction Section1 The Ancient Universe Section2 The Enduring Earth-Centered System Section3 The Sun Takes
    [Show full text]
  • Exoplanet Community Report
    JPL Publication 09‐3 Exoplanet Community Report Edited by: P. R. Lawson, W. A. Traub and S. C. Unwin National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Pasadena, California March 2009 The work described in this publication was performed at a number of organizations, including the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). Publication was provided by the Jet Propulsion Laboratory. Compiling and publication support was provided by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not constitute or imply its endorsement by the United States Government, or the Jet Propulsion Laboratory, California Institute of Technology. © 2009. All rights reserved. The exoplanet community’s top priority is that a line of probe­class missions for exoplanets be established, leading to a flagship mission at the earliest opportunity. iii Contents 1 EXECUTIVE SUMMARY.................................................................................................................. 1 1.1 INTRODUCTION...............................................................................................................................................1 1.2 EXOPLANET FORUM 2008: THE PROCESS OF CONSENSUS BEGINS.....................................................2
    [Show full text]
  • Estimation of the XUV Radiation Onto Close Planets and Their Evaporation⋆
    A&A 532, A6 (2011) Astronomy DOI: 10.1051/0004-6361/201116594 & c ESO 2011 Astrophysics Estimation of the XUV radiation onto close planets and their evaporation J. Sanz-Forcada1, G. Micela2,I.Ribas3,A.M.T.Pollock4, C. Eiroa5, A. Velasco1,6,E.Solano1,6, and D. García-Álvarez7,8 1 Departamento de Astrofísica, Centro de Astrobiología (CSIC-INTA), ESAC Campus, PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain e-mail: [email protected] 2 INAF – Osservatorio Astronomico di Palermo G. S. Vaiana, Piazza del Parlamento, 1, 90134, Palermo, Italy 3 Institut de Ciènces de l’Espai (CSIC-IEEC), Campus UAB, Fac. de Ciències, Torre C5-parell-2a planta, 08193 Bellaterra, Spain 4 XMM-Newton SOC, European Space Agency, ESAC, Apartado 78, 28691 Villanueva de la Cañada, Madrid, Spain 5 Dpto. de Física Teórica, C-XI, Facultad de Ciencias, Universidad Autónoma de Madrid, Cantoblanco, 28049 Madrid, Spain 6 Spanish Virtual Observatory, Centro de Astrobiología (CSIC-INTA), ESAC Campus, Madrid, Spain 7 Instituto de Astrofísica de Canarias, 38205 La Laguna, Spain 8 Grantecan CALP, 38712 Breña Baja, La Palma, Spain Received 27 January 2011 / Accepted 1 May 2011 ABSTRACT Context. The current distribution of planet mass vs. incident stellar X-ray flux supports the idea that photoevaporation of the atmo- sphere may take place in close-in planets. Integrated effects have to be accounted for. A proper calculation of the mass loss rate through photoevaporation requires the estimation of the total irradiation from the whole XUV (X-rays and extreme ultraviolet, EUV) range. Aims. The purpose of this paper is to extend the analysis of the photoevaporation in planetary atmospheres from the accessible X-rays to the mostly unobserved EUV range by using the coronal models of stars to calculate the EUV contribution to the stellar spectra.
    [Show full text]
  • Vega Ground Segment General Presentation
    CENTRE NATIONAL D'ETUDES SPATIALES CODE IDENTIFICATION PROJET VG-NT-2-C-0012-CNES EDITION : 1 REVISION : 0 Sous-Direction Développements Sol Date édition ou dernière révision :11/02/2003 18, Avenue Edouard-Belin 31401 TOULOUSE Cedex 4 REF. D'AUTEUR :SDS/PL/SV/2003-00048 CLASSE : 1 CATEGORIE : 1 Rond-point de l'Espace 91023 EVRY Cedex RESERVE A L'INDUSTRIEL SDS/G BP 254 - 97377 KOUROU CEDEX PROJET : VEGA GROUND SEGMENT TITRE DU DOCUMENT : VEGA GROUND SEGMENT GENERAL PRESENTATION NOM & FONCTION DATE & SIGNATURE LISTE DE DIFFUSION Nb A I SDS/PL 1 X SDS/SM 1 X SDS/AP 1 X PREPARE Project Team PAR : SDS/SG 1 X SDS/G 1 X SDS/D + DA 1 X DLA/RAP/ADS 1 X DLA/SDT/SP 1 X POUR DLA/D 1 X APPROBATION : ESA/LAU-V/IPT M. CARDONE 1 X ESA/IMT Mme. CROWTHER 1 X POUR ACCEPTATION : APPLICATION AUTORISEE Marc VALES PAR : Project Coordinator A=Action I=Information VG-NT-2-C-0012-CNES-eng.doc Version validée SDS Imprimé le 16 / 04 / 03 CENTRE NATIONAL D'ETUDES SPATIALES CODE IDENTIFICATION PROJET VG-NT-2-C-0012-CNES Sous-Direction Développements Sol FICHE 18, Avenue Edouard-Belin 31401 TOULOUSE Cedex 4 SIGNALETIQUE Rond-point de l'Espace 91023 EVRY Cedex FICHIER INFORMATIQUE SDS/G BP 254 - 97377 KOUROU CEDEX C:\WINNT\Profiles\Commun\Bureau\VEGA\Vega Anglais\SVMV0004803.10A.doc LANGUE : EDITION : REVISION : Fr 1 0 Nombre de pages totales (y/c annexes Nb de pages et pages de garde) : 24 annexes : DATE D'EDITION OU DERNIERE REVISION : 11/02/2003 TITRE : VEGA GROUND SEGMENT GENERAL PRESENTATION NOM (S) AUTEUR (S) TYPE DE DOCUMENT Project Team NOTE TECHNIQUE CLASSEMENT PHYSIQUE N° MARCHE CLASSE : 1 CATEGORIE : 1 RESUME D'AUTEUR Presentation of the VEGA Ground Segment design.
    [Show full text]
  • 2020-08-24-Final Amended Complaint
    Case: 3:20-cv-00374-jdp Document #: 27 Filed: 08/24/20 Page 1 of 32 UNITED STATES DISTRICT COURT WESTERN DISTRICT OF WISCONSIN LUCIANNE M. WALKOWICZ, ) AMENDED COMPLAINT ) Plaintiff, ) ) v. ) CASE NO. 3:20-cv-00374-jdp ) AMERICAN GIRL, LLC1, AMERICAN GIRL ) BRANDS, LLC, and MATTEL, INC. ) ) Defendants. ) JURY DEMAND AMENDED COMPLAINT NOW COMES the PLAINTIFF LUCIANNE M. WALKOWICZ (“Plaintiff” or “Dr. Walkowicz” or “Lucianne”), by and through her attorneys, Mudd Law Offices, and complains of DEFENDANTS AMERICAN GIRL, LLC, AMERICAN GIRL BRANDS, LLC, and MATTEL, INC. (collectively, “Defendants”), and states as follows: NATURE OF ACTION 1. This is an action for the violation of right of publicity, false designation of origin in violation of 15 U.S.C. § 1125(a), unfair competition, and related claims. 2. By this action, Dr. Walkowicz seeks compensatory damages, punitive damages, statutory damages, reasonable attorney’s fees and costs, injunctive relief, and all other relief to which Lucianne may be entitled as a matter of law. PARTIES 3. Dr. Walkowicz is a citizen of the State of Illinois and a resident of Cook County, 1 In their Motion to Dismiss the Complaint, the Defendants explain that American Girl, Inc. converted to American Girl, LLC. Based on this representation, the Plaintiff has changed the entity name accordingly. Case: 3:20-cv-00374-jdp Document #: 27 Filed: 08/24/20 Page 2 of 32 Illinois. 4. American Girl, LLC is a Delaware corporation with its principal place of business in Middleton, Wisconsin. 5. American Girl Brands, LLC is a Delaware corporation with its principal place of business in Middleton, Wisconsin.
    [Show full text]