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Low Thrust Manoeuvres to Perform Large Changes of RAAN Or Inclination in LEO
Facoltà di Ingegneria Corso di Laurea Magistrale in Ingegneria Aerospaziale Master Thesis Low Thrust Manoeuvres To Perform Large Changes of RAAN or Inclination in LEO Academic Tutor: Prof. Lorenzo CASALINO Candidate: Filippo GRISOT July 2018 “It is possible for ordinary people to choose to be extraordinary” E. Musk ii Filippo Grisot – Master Thesis iii Filippo Grisot – Master Thesis Acknowledgments I would like to address my sincere acknowledgments to my professor Lorenzo Casalino, for your huge help in these moths, for your willingness, for your professionalism and for your kindness. It was very stimulating, as well as fun, working with you. I would like to thank all my course-mates, for the time spent together inside and outside the “Poli”, for the help in passing the exams, for the fun and the desperation we shared throughout these years. I would like to especially express my gratitude to Emanuele, Gianluca, Giulia, Lorenzo and Fabio who, more than everyone, had to bear with me. I would like to also thank all my extra-Poli friends, especially Alberto, for your support and the long talks throughout these years, Zach, for being so close although the great distance between us, Bea’s family, for all the Sundays and summers spent together, and my soccer team Belfiga FC, for being the crazy lovable people you are. A huge acknowledgment needs to be address to my family: to my grandfather Luciano, for being a great friend; to my grandmother Bianca, for teaching me what “fighting” means; to my grandparents Beppe and Etta, for protecting me -
Observing from Space Orbits, Constraints, Planning, Coordination
Observing from Space Orbits, constraints, planning, coordination Integral XMM-Newton Jan-Uwe Ness European Space Astronomy Centre (ESAC) Villafranca del Castillo, Spain On behalf of the Integral and XMM-Newton Science Operations Centres Slide 1 Observing from Space - Orbits http://sci.esa.int/integral/59688-integral-fifteen-years-in-orbit/ Slide 2 Observing from Space - Orbits Highly elliptical Earth orbit: XMM-Newton, Integral, Chandra Slide 3 Observing from Space - Orbits Low-Earth orbit: ~1.5 hour, examples: Hubble Space Telescope Swift NuSTAR Fermi Earth blocking, especially low declination objects Only short snapshots of a few 100s possible No long uninterrupted observations Only partial overlap with Integral/XMM possible Slide 4 Observing from Space - Orbits Orbit around Lagrange point L2 past: future: Herschel James Webb Planck Athena present: Gaia Slide 5 Observing from Space – Constraints Motivations for constraints: • Safety of space-craft and instruments • Contamination by bright optical/X-ray sources or straylight from them • Functionality of star Tracker • Power supply (solar panels) • Thermal stability (avoid heat from the sun) • Ground contact for remote commanding and downlink of data Space-specific constraints in bold orange Slide 6 Observing from Space – Constraints Examples for constraints: • No observations while passing through radiation belts • Orientation of space craft to sun • Large avoidance angles around Sun and anti-Sun, Moon, Earth, Bright planets • No slewing over Moon and Earth (planets ok) • Availability -
Javier Peralta Calvillo Generated From: Editor CVN De FECYT Date of Document: 24/01/2021 V 1.4.3 4154B7e2be6a86b67f637261e4ad3d11
Javier Peralta Calvillo Generated from: Editor CVN de FECYT Date of document: 24/01/2021 v 1.4.3 4154b7e2be6a86b67f637261e4ad3d11 This electronic file (PDF) has embedded CVN technology (CVN-XML). The CVN technology of this file allows you to export and import curricular data from and to any compatible data base. List of adapted databases available at: http://cvn.fecyt.es/ 4154b7e2be6a86b67f637261e4ad3d11 General quality indicators of scientific research This section describes briefly the main quality indicators of scientific production (periods of research activity, experience in supervising doctoral theses, total citations, articles in journals of the first quartile, H index...). It also includes other important aspects or peculiarities. My name is Javier Peralta and I was born in Algeciras (1979, Spain). I graduated in Physics at the University of La Laguna (Spain) in 2003, specializing in the fields of Astrophysics and Applied Physics. In 2009, I got an European PhD degree in Physics at the University of the Basque Country (Spain) with the highest qualification ("Cum Laude") . My PhD research, supervised by Professors Agustín Sánchez-Lavega and Ricardo Hueso, focused on the atmospheric dynamics of the planet Venus using data from the space missions Galileo and Venus Express. As a result, 6 articles were published in international peer review journals (4 of them as first author) along with more than 80 citations which allowed to be awarded in 2012 with the “Extraordinary Prize of Doctorate” granted by the University of the Basque Country. After my PhD, I spent the last 10 years (2009-2019) working in different research institutions as postdoctoral researcher: 2 years at IAA/CSIC in Granada (Spain), 3 years at the Astronomical Observatory of Lisbon (CAAUL/OAL, Portugal) and 5 years at the Institute of Space and Astronautical Science of Japan (ISAS/JAXA), funded by JAXA's International Top Young Fellowship (ITYF). -
NASA Process for Limiting Orbital Debris
NASA-HANDBOOK NASA HANDBOOK 8719.14 National Aeronautics and Space Administration Approved: 2008-07-30 Washington, DC 20546 Expiration Date: 2013-07-30 HANDBOOK FOR LIMITING ORBITAL DEBRIS Measurement System Identification: Metric APPROVED FOR PUBLIC RELEASE – DISTRIBUTION IS UNLIMITED NASA-Handbook 8719.14 This page intentionally left blank. Page 2 of 174 NASA-Handbook 8719.14 DOCUMENT HISTORY LOG Status Document Approval Date Description Revision Baseline 2008-07-30 Initial Release Page 3 of 174 NASA-Handbook 8719.14 This page intentionally left blank. Page 4 of 174 NASA-Handbook 8719.14 This page intentionally left blank. Page 6 of 174 NASA-Handbook 8719.14 TABLE OF CONTENTS 1 SCOPE...........................................................................................................................13 1.1 Purpose................................................................................................................................ 13 1.2 Applicability ....................................................................................................................... 13 2 APPLICABLE AND REFERENCE DOCUMENTS................................................14 3 ACRONYMS AND DEFINITIONS ...........................................................................15 3.1 Acronyms............................................................................................................................ 15 3.2 Definitions ......................................................................................................................... -
Lagrange Remote Sensing Instruments: the Extreme Ultraviolet Imager (Euvi)
LAGRANGE REMOTE SENSING INSTRUMENTS: THE EXTREME ULTRAVIOLET IMAGER (EUVI) C. Kintziger (CSL) - Presenter S. Habraken (CSL) P. Bouchez (CSL) Matthew West (ROB) David Berghmans (ROB) Manfred Gyo (PMOD/WRC) Margit Haberreiter (PMOD/WRC) Jackie Davies (RAL Space) Martin Caldwell (RAL Space) Ian Tosh (RAL Space) Stefan Kraft (ESA) 1 ESWW 2018, 9 Nov. 2018 LGRRS-EUVI | Mission overview 4 remote-sensing instruments See Poster 23 by J. Davies 2 ESWW 2018, 9 Nov. 2018 LGRRS-EUVI | Mission overview 5 in-situ instruments 3 ESWW 2018, 9 Nov. 2018 LGRRS-EUVI | Mission overview • Overall Remote Sensing Instruments leader: RAL Space (UK) • EUVI study led by three institutes: – CSL (BE) – ROB (BE) – PMOD/WRC (CH) • CSL activities • ROB activities • PMOD activities – EUVI Instrument manager: – instrument – electrical engineering • Overall management requirements – mechanisms • System study – instrument operation – mechanical engineering • Optical engineering – ground segments • Thermal engineering • AIT engineering • Roles & Responsibilities – BPI: Pr. Dr. Serge Habraken (CSL) – Bco-I: Dr. Matthew J West (ROB) – CSL work funded by Belspo via Prodex Programme 4 ESWW 2018, 9 Nov. 2018 LGRRS-EUVI | Mission overview • EUV Imager – SSA programme (SWE) – Location: L5 – Goal: image the full solar disc – Waveband: EUV wavelength (e.g. 193 Å) – Heritage: PROBA-2 SWAP ESIO (GSTP) Solar Orbiter EUI Parameter Requirement Spectral resolution < 1.5 푛푚 퐹푊퐻푀 Spatial resolution < 5 푎푟푐푠푒푐 Field of view 42.6′ 푥 42.6′ Mass < 8 푘푔 Size < 600 푥 150 푥 150 푚푚 Power < 10 푊 5 ESWW 2018, 9 Nov. 2018 LGRRS-EUVI | Instrument overview • Selected wavelengths 131 nm 19.5 nm 30.4 nm Semi-Static Structures Dynamic structures Regions Filaments/Prominences Flares Chromosphere Active Regions Eruptions Million Degree Corona Coronal Holes EUV Waves Dimmings 6 ESWW 2018, 9 Nov. -
FINESSE and ARIEL + CASE: Dedicated Transit Spectroscopy Missions for the Post-TESS Era
FINESSE and ARIEL + CASE: Dedicated Transit Spectroscopy Missions for the Post-TESS Era Fast Infrared Exoplanet FINESSE Spectroscopy Survey Explorer Exploring the Diversity of New Worlds Around Other Stars Origins | Climate | Discovery Jacob Bean (University of Chicago) Presented on behalf of the FINESSE/CASE science team: Mark Swain (PI), Nicholas Cowan, Jonathan Fortney, Caitlin Griffith, Tiffany Kataria, Eliza Kempton, Laura Kreidberg, David Latham, Michael Line, Suvrath Mahadevan, Jorge Melendez, Julianne Moses, Vivien Parmentier, Gael Roudier, Evgenya Shkolnik, Adam Showman, Kevin Stevenson, Yuk Yung, & Robert Zellem Fast Infrared Exoplanet FINESSE Spectroscopy Survey Explorer Exploring the Diversity of New Worlds Around Other Stars **Candidate NASA MIDEX mission for launch in 2023** Objectives FINESSE will test theories of planetary origins and climate, transform comparative planetology, and open up exoplanet discovery space by performing a comprehensive, statistical, and uniform survey of transiting exoplanet atmospheres. Strategy • Transmission spectroscopy of 500 planets: Mp = few – 1,000 MEarth • Phase-resolved emission spectroscopy of a subset of 100 planets: Teq > 700 K • Focus on synergistic science with JWST: homogeneous survey, broader context, population properties, and bright stars Hardware • 75 cm aluminum Cassegrain telescope at L2 • 0.5 – 5.0 μm high-throughput prism spectrometer with R > 80 • Single HgCdTe detector with JWST heritage for science and guiding Origins | Climate | Discovery Advantages of Fast Infrared -
Arxiv:2010.15996V1 [Astro-Ph.IM] 29 Oct 2020 Keywords: ARIEL, Exoplanets, Transit Photometry, Light Curves, Stellar Spots, Machine Learning
Draft version November 2, 2020 Typeset using LATEX default style in AASTeX63 Lessons Learned from the 1st ARIEL Machine Learning Challenge: Correcting Transiting Exoplanet Light Curves for Stellar Spots Nikolaos Nikolaou ,1 Ingo P. Waldmann ,1 Angelos Tsiaras ,1 Mario Morvan ,1 Billy Edwards ,1 Kai Hou Yip ,1 Giovanna Tinetti ,1 Subhajit Sarkar,2 James M. Dawson,2 Vadim Borisov,3 Gjergji Kasneci,3 Matej Petkovic,´ 4 Tomaˇz Stepiˇsnik,4 Tarek Al-Ubaidi,5, 6 Rachel Louise Bailey ,6 Michael Granitzer ,7 Sahib Julka ,7 Roman Kern,8 Patrick Ofner ,8 Stefan Wagner,9 Lukas Heppe ,10 Mirko Bunse ,10 and Katharina Morik 10 1Department of Physics and Astronomy, University College London, Gower Street, London, WC1E 6BT, UK 2School of Physics and Astronomy, Cardiff University, The Parade, Cardiff, CF24 3AA, UK 3Department of Computer Science, University of Tuebingen, Tuebingen, Germany 4Joˇzef Stefan Institute, Ljubljana, Slovenia 5DCCS, Austria 6Space Research Institute, Austrian Academy of Sciences, Austria 7Chair of Data Science, University of Passau, Germany 8Know-Center GmbH - Research Center for Data-Driven Business & Big Data Analytics, Austria 9Commission for Astronomy, Austrian Academy of Sciences, Graz, Austria 10Artificial Intelligence Group, TU Dortmund University, Germany Submitted to ApJ ABSTRACT The last decade has witnessed a rapid growth of the field of exoplanet discovery and characterisation. However, several big challenges remain, many of which could be addressed using machine learning methodology. For instance, the most prolific method for detecting exoplanets and inferring several of their characteristics, transit photometry, is very sensitive to the presence of stellar spots. The current practice in the literature is to identify the effects of spots visually and correct for them manually or discard the affected data. -
INNER WORKINGS Inner Workings: Hubble’S Quarter Century in Orbit Has Opened a Universe of Possibilities David J
INNER WORKINGS Inner Workings: Hubble’s quarter century in orbit has opened a universe of possibilities David J. Harris Science Writer advocates, including astronomers John Bahcall and Lyman Spitzer, in 1974 obtained a letter from the National Research Council’s decadal survey of astronomy committee saying that When the Hubble Space Telescope was beyond the present orbiting astronomical ob- an updated 1970 survey would rank the proj- deployed from Space Shuttle Discovery on servatories program” (1). This new breed of ect higher. That gave them the leverage they April 25, 1990, few knew just how far-reach- telescope would have a much larger aperture needed to convince Congress. ing its impact would be on astronomy, cos- than existing orbiting astronomical observa- The initial proposed launch date was 1983. mology, and public appreciation of the tories and be capable of “stellar and nebular But technical delays, budget problems, and universe. “It has given us views of the uni- studies through the entire spectral range from the 1986 Space Shuttle Challenger disaster verse that we have never seen before and soft X rays to infrared.” However, the budgets pushed the launch to 1990. Then came a se- provided a wealth of data for astronomers and the technological capabilities of the ries of difficult servicing missions beginning around the world to ponder,” says Ken time presented challenges for a large-aper- in 1993 to install corrective optics for the in- Sembach, head of the Hubble Mission Office ture space telescope. correctly ground main mirror and upgrade at the Space Telescope Science Institute. Hub- Recommendations at the Academy’s1965 various components. -
Exploring the Solar Poles and the Heliosphere from High Helio-Latitude
A white paper submitted to ESA for the Voyage 2050 long- term plan ? A journey to the polar regions of a star: Exploring the solar poles and the heliosphere from high helio-latitude Louise Harra ([email protected]) and the solar polar team PMOC/WRC, Dorfstrasse 33, CH-7260 Davos Dorf & ETH-Zürich, Switzerland [Image: Polar regions of major Solar System bodies. Top left, clockwise - Near-surface zonal flows around the solar north pole Bogart et al. (2015); Earth’s changing magnetic field from ESA’s Swarm constellation; Southern polar cap of Mars from ESA’s ExoMars; Jupiter’s poles from the NASA Juno mission; Saturn’s poles from the NASA Cassini mission.] Overview We aim to embark on one of humankind’s great journeys – to travel over the poles of our star, with a spacecraft unprecedented in its technology and instrumentation – to explore the polar regions of the Sun and their effect on the inner heliosphere in which we live. The polar vantage point provides a unique opportunity for major scientific advances in the field of heliophysics, and thus also provides the scientific underpinning for space weather applications. It has long been a scientific goal to study the poles of the Sun, illustrated by the NASA/ESA International Solar Polar Mission that was proposed over four decades ago, which led to the flight of ESA’s Ulysses spacecraft (1990 to 2009). Indeed, with regard to the Earth, we took the first tentative steps to explore the Earth’s polar regions only in the 1800s. Today, with the aid of space missions, key measurements relating to the nature and evolution of Earth’s polar regions are being made, providing vital input to climate-change models. -
ASTRONOMY 18 Th-Century Math Sets Stage for Future Space Exploration Columbus Dispatch Tuesday, October 05, 2004 TOM BURNS
ASTRONOMY 18 th-century math sets stage for future space exploration Columbus Dispatch Tuesday, October 05, 2004 TOM BURNS In the mid-18 th century, mathematicians and scientists such as J.L. Lagrange were obsessed with the three-body problem - mathematical rules behind the mutual attraction of three large bodies, such as two planets orbiting the sun or a moon orbiting a planet orbiting the sun. Almost 250 years later, Lagrange's elegant solution has implications that will determine the course of space exploration over the coming decades. It works like this: If one object orbits another, there are five places near the orbiting object where another object can lock into a stable and permanent orbit. Think of them as naturalgravity wells. To put a space station in a stable orbit near Earth, the No. 4 and No. 5 sun-Earth natural-gravity wells - known as Lagrange points - can't be beat. They are located along Earth's orbit 60 degrees on either side of Earth. One precedes Earth and the other trails it. Unfortunately, they are each 50 million miles from our planet, a bit distant for things such as supply shipments, rescues and maintenance missions. Much better is Lagrange point No. 3, about 1 million miles toward the sun. At that location, your space telescope is locked as a minor planet orbiting the sun. But because of its sunny location, Lagrange point No. 3 is not a great place to observe stars. However, the No. 3 Solar and Heliospheric Observatory, or SoHo, has for years produced beautiful images of our home star. -
Mathematics for Physics I
Mathematics for Physics I A set of lecture notes by Michael Stone PIMANDER-CASAUBON Alexandria Florence London • • ii Copyright c 2001,2002 M. Stone. All rights reserved. No part of this material can be reproduced, stored or transmitted without the written permission of the author. For information contact: Michael Stone, Loomis Laboratory of Physics, University of Illinois, 1110 West Green Street, Urbana, IL 61801, USA. Preface These notes were prepared for the first semester of a year-long mathematical methods course for begining graduate students in physics. The emphasis is on linear operators and stresses the analogy between such operators acting on function spaces and matrices acting on finite dimensional spaces. The op- erator language then provides a unified framework for investigating ordinary and partial differential equations, and integral equations. The mathematical prerequisites for the course are a sound grasp of un- dergraduate calculus (including the vector calculus needed for electricity and magnetism courses), linear algebra (the more the better), and competence at complex arithmetic. Fourier sums and integrals, as well as basic ordinary differential equation theory receive a quick review, but it would help if the reader had some prior experience to build on. Contour integration is not required. iii iv PREFACE Contents Preface iii 1 Calculus of Variations 1 1.1 What is it good for? . 1 1.2 Functionals . 2 1.2.1 The functional derivative . 2 1.2.2 The Euler-Lagrange equation . 3 1.2.3 Some applications . 4 1.2.4 First integral . 8 1.3 Lagrangian Mechanics . 9 1.3.1 One degree of freedom . -
GNSS in Space Part 1 Formation Flying Radio Frequency Missions, Techniques, and Technology
WORKING PAPERS GNSS in Space Part 1 Formation Flying Radio Frequency Missions, Techniques, and Technology FIGURE 1 PRISMA satellites (SSC image) Using two or more small satellites can sometimes be better than one, especially when trying to create a large spaceborne instrument for scientific research or experiments.B ut coordinating the alignment of the components of such instruments on separate space vehicles requires highly accurate orientation and positioning. Carrier phase GNSS can provide such precision for spacecraft operating below the altitude of GPS satellites, and GNSS-like techniques can be employed for spacecraft operating in higher orbits. THOMAS GRELIER ormation flying (FF) creates large easiest way because most LEO satellites CENTRE NAtional d’ETUDES SPATIALES (CNES) spaceborne instruments by using are already provided with a GPS or ALBERTO GARCIA several smaller satellites in close GLONASS receiver for orbit and time EUROPEAN SPACE AGENCY (ESA) Fformation. The concept requires determination. very accurate relative positioning and Thanks to GNSS constellations, for- ERIC PÉRAGIN, LAURENT LEstARQUIT, JON HARR, orientation of the spacecrafts, the com- mation flying can be made at higher alti- DOMINIQUE SEGUELA , JEAN-LuC ISSLER plexity of which is largely outweighed tudes with a perigee of up to 25,000 kilo- CNES by the enormous benefit of the extended meters, if GNSS receivers equipped with instrument size compared to traditional low acquisition and tracking thresholds JEAN-BAPTIstE THEVENET, NICOLAS PERRIAULT, one-satellite configurations. are selected. Such receivers have tight CHRIstIAN MEHLEN, CHRIstOPHE ENSENAT, The easiest way to perform forma- coupling between the signal processing NICOLAS WILHELM, ANA-MARIA BADIOLA tion flying with relative attitude and and the onboard orbital Kalman filter MARTINEZ positioning in space is to use signals delivering pseudovelocity and pseudo- THALES ALENIA SPACE broadcast by GNSS satellites.