DOCSLIB.ORG

Research and Scientific Support Department 2003 – 2004

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Research and Scientific Support Department 2003 – 2004 COVER 7/11/05 4:55 PM Page 1 SP-1288 SP-1288 Research and Scientific Research Report on the activities of the Support Department Research and Scientific Support Department 2003 – 2004 Contact: ESA Publications Division c/o ESTEC, PO Box 299, 2200 AG Noordwijk, The Netherlands Tel. (31) 71 565 3400 - Fax (31) 71 565 5433 Sec1.qxd 7/11/05 5:09 PM Page 1 SP-1288 June 2005 Report on the activities of the Research and Scientific Support Department 2003 – 2004 Scientific Editor A. Gimenez Sec1.qxd 7/11/05 5:09 PM Page 2 2 ESA SP-1288 Report on the Activities of the Research and Scientific Support Department from 2003 to 2004 ISBN 92-9092-963-4 ISSN 0379-6566 Scientific Editor A. Gimenez Editor A. Wilson Published and distributed by ESA Publications Division Copyright © 2005 European Space Agency Price €30 Sec1.qxd 7/11/05 5:09 PM Page 3 3 CONTENTS 1. Introduction 5 4. Other Activities 95 1.1 Report Overview 5 4.1 Symposia and Workshops organised 95 by RSSD 1.2 The Role, Structure and Staffing of RSSD 5 and SCI-A 4.2 ESA Technology Programmes 101 1.3 Department Outlook 8 4.3 Coordination and Other Supporting 102 Activities 2. Research Activities 11 Annex 1: Manpower Deployment 107 2.1 Introduction 13 2.2 High-Energy Astrophysics 14 Annex 2: Publications 113 (separated into refereed and 2.3 Optical/UV Astrophysics 19 non-refereed literature) 2.4 Infrared/Sub-millimetre Astrophysics 22 2.5 Solar Physics 26 Annex 3: Seminars and Colloquia 149 2.6 Heliospheric Physics/Space Plasma Studies 31 2.7 Comparative Planetology and Astrobiology 35 Annex 4: Acronyms 153 2.8 Minor Bodies 39 2.9 Fundamental Physics 43 2.10 Research Activities in SCI-A 45 3. Scientific Support Activities 53 3.1 Astrophysics Missions Division 56 3.2 Solar and Solar-Terrestrial 64 Missions Division 3.3 Planetary Missions Division 70 3.4 Fundamental Physics Missions Division 78 3.5 Space Telescope Operations Division 80 3.6 Science Operations and Data Systems 83 Division 3.7 Science Payload and Advanced Concepts 89 Office Sec1.qxd 7/11/05 5:09 PM Page 5 introduction 5 1. INTRODUCTION 1.1 Report Overview workshops organised by the Department, support to the Directorate’s science communication activities, and This report on the activities of the Research and various other activities. Scientific Support Department (RSSD) covers the 2-year period of 2003-2004. It is prepared as input to the While this Biennial Report provides perspective on the Department’s Advisory Committee, a group of breadth and quality of the activities of the staff, both in independent external scientists invited by the Director of their research and functional work, it is not intended to be ESA’s Scientific Programme to review the Department’s comprehensive. Up-to-date information on the Depart- activities. It forms the basis of the oral reports made to ment’s activities can be obtained at http://www.rssd. ESA’s Space Science Advisory Committee and the esa.int and for SCI-A at http://sci.esa.int/science-e/ Science Programme Committee every second www/area/index.cfm?fareaid=65 year. Through the publication of the report as an ‘SP’ (Special Publication) by the ESA Publications Division, the activities of the Department are brought to the 1.2 The Role, Structure and Staffing of RSSD attention of the scientific community and to a broader and SCI-A audience. RSSD, one of the two Departments of ESA’s Scientific These Biennial Reports have been produced since 1980. Directorate, provides the direct interface to the scientific In this volume, a number of changes introduced in the community throughout all mission phases. Following last report have been kept. The report also covers the in-orbit checkout and commissioning, it is also respons- activities of the Science Payload and Advanced Concepts ible for the management of the missions. In addition, the Office (SCI-A) owing to its close links with many Department plays its part in the dissemination of activities in RSSD and its history as the previous Science scientific knowledge to the public and for educational Payload Technology Division. purposes. The report is divided into four Chapters plus four In essence, the role of RSSD is to ensure the best possible Annexes. Chapter 1 deals with the Department’s role and scientific performance of ESA’s Scientific Programme organisation. A brief summary is given because its missions. To this end, the Department is responsible for mandate and structure did not change significantly the implementation of all science management aspects of during the reporting period. Reference should be made to the missions in the Science Directorate throughout their the previous report (ESA SP-1268) for further study and operations phases. information. The names of staff, their locations, their functional duties and scientific research interests are In particular, the Department is responsible for providing given in Annex 1. scientific expertise to studies and projects in all phases, and for ensuring that maximum scientific return within Chapter 2 addresses the scientific research of the practical technical and budgetary constraints is Department’s staff, broken down according to maintained as a target through all phases of a scientific ‘discipline’ rather than divisional structure. A complete mission. The Department also manages, through its study listing of the scientific papers published in the literature or project scientists, the activities of each mission is given in Annex 2. Some 340 refereed papers were science team. published during 2003 and 2004, and more than 350 conference papers and other publications appeared. RSSD is responsible for all aspects of science operations (definition, development, implementation and execution) Chapter 3 provides a top-level summary of the mission- through all phases of missions and manages the related activities at Divisional level. For the four operations phases of missions following in-orbit Missions Divisions, the prime contributions to the commissioning, supported, as necessary, by system scientific support of the various elements of the Science engineering expertise from the Scientific Projects Programme are summarised. For the two Operations Department. Support Divisions, special mention is also made of post- operational and archiving phases. The activities of SCI-A In very close coordination with SCI-A, RSSD provides are included. scientific and payload expertise within the Agency in all phases of scientific missions, including to other Finally, Chapter 4 addresses a variety of activities carried directorates of the Agency (e.g. on International Space out by RSSD in its support role to the community. The Station payloads). It works with external science teams Chapter summarises important scientific symposia and to define the science requirements for future mission Sec1.qxd 7/11/05 5:09 PM Page 6 6 introduction Head of Research and Scientific Support future missions as well for new payload technologies in Department support of the Cosmic Vision long-term Scientific SCI-S Programme. The Office works, in close liaison with the RSSD study scientists and the science community, to Chief Scientist SCI-SR determine the science and technological needs of this programme. In addition, SCI-A provides payload support/expertise to missions under development, both to RSSD Project Scientists as well as the Science Projects Astrophysics Missions Science Operations and Division Data Systems Division Department. The Office is also responsible for laboratory SCI-SA SCI-SD support throughout the Directorate, including those Planetary Missions Space Telescope RSSD research activities requiring such support. Division Operations Division SCI-SB SCI-SN The organigram of RSSD is shown in Fig. 1.2/1. In Solar & Solar-Terrestrial addition, the office of the Department Head is supported Missions Division SCI-SH by a budget control group including three integrated project controllers from SCI-M. The role and functions Fundamental Physics Missions Division of the six Divisions, and those of SCI-A, are described SCI-SP further in Chapter 3. Figure 1.2/1: The structure of RSSD. The staff of the Department (37 at the end of 2004) and of SCI-A (21, including 2 advanced recruitments) hold posts within the overall ESA staff complement. Staff associated with Science Operations Teams are generally studies and associated payloads and passes these to supernumerary positions. By the end of 2004, there was SCI-A for follow-up. a complement of 68 supernumeraries (3 in SCI-A). Fig. 1.2/2 depicts the structure of SCI-A. It should be It is, of course, very important that the scientific staff of noted that, in these teams, many contractors and often both RSSD and SCI-A maintain their scientific staff from Principal Investigator (PI) institutes work proficiency by undertaking personal research. together in an integrated structure. An overview of the staff in post at the end of 2004 is given in Table 1, In order to discharge its responsibilities and tasks in an integrating personnel from RSSD proper and SCI-A. efficient manner, the Department is structured into four Figure 1.2/3 gives the distribution of staff according to Missions Divisions: functions within RSSD. — the Astrophysics Missions Division; Department staff are located not only at ESTEC, close to — the Planetary Missions Division; the Science Directorate’s project teams and the Technical — the Solar and Solar-Terrestrial Missions Division; Directorate, but also in Villafranca (ISO and XXM- — the Fundamental Physics Missions Division; Newton science operations teams), in Garching and Baltimore (Space Telescope Operations Division) and and two Operations Support Divisions: Greenbelt (SOHO Project Scientist Team at NASA Goddard Space Flight Center). During 2004, the Villa- — the Science Operations and Data Systems Division; franca facilities were integrated into the European Space — the Space Telescope Operations Division.
Load more

Recommended publications
  • ESA Missions AO Analysis
    ESA Announcements of Opportunity Outcome Analysis Arvind Parmar Head, Science Support Office ESA Directorate of Science With thanks to Kate Isaak, Erik Kuulkers, Göran Pilbratt and Norbert Schartel (Project Scientists) ESA UNCLASSIFIED - For Official Use The ESA Fleet for Astrophysics ESA UNCLASSIFIED - For Official Use Dual-Anonymous Proposal Reviews | STScI | 25/09/2019 | Slide 2 ESA Announcement of Observing Opportunities Ø Observing time AOs are normally only used for ESA’s observatory missions – the targets/observing strategies for the other missions are generally the responsibility of the Science Teams. Ø ESA does not provide funding to successful proposers. Ø Results for ESA-led missions with recent AOs presented: • XMM-Newton • INTEGRAL • Herschel Ø Gender information was not requested in the AOs. It has been ”manually” derived by the project scientists and SOC staff. ESA UNCLASSIFIED - For Official Use Dual-Anonymous Proposal Reviews | STScI | 25/09/2019 | Slide 3 XMM-Newton – ESA’s Large X-ray Observatory ESA UNCLASSIFIED - For Official Use Dual-Anonymous Proposal Reviews | STScI | 25/09/2019 | Slide 4 XMM-Newton Ø ESA’s second X-ray observatory. Launched in 1999 with annual calls for observing proposals. Operational. Ø Typically 500 proposals per XMM-Newton Call with an over-subscription in observing time of 5-7. Total of 9233 proposals. Ø The TAC typically consists of 70 scientists divided into 13 panels with an overall TAC chair. Ø Output is >6000 refereed papers in total, >300 per year ESA UNCLASSIFIED - For Official Use
    [Show full text]
  • No. 40. the System of Lunar Craters, Quadrant Ii Alice P
    NO. 40. THE SYSTEM OF LUNAR CRATERS, QUADRANT II by D. W. G. ARTHUR, ALICE P. AGNIERAY, RUTH A. HORVATH ,tl l C.A. WOOD AND C. R. CHAPMAN \_9 (_ /_) March 14, 1964 ABSTRACT The designation, diameter, position, central-peak information, and state of completeness arc listed for each discernible crater in the second lunar quadrant with a diameter exceeding 3.5 km. The catalog contains more than 2,000 items and is illustrated by a map in 11 sections. his Communication is the second part of The However, since we also have suppressed many Greek System of Lunar Craters, which is a catalog in letters used by these authorities, there was need for four parts of all craters recognizable with reasonable some care in the incorporation of new letters to certainty on photographs and having diameters avoid confusion. Accordingly, the Greek letters greater than 3.5 kilometers. Thus it is a continua- added by us are always different from those that tion of Comm. LPL No. 30 of September 1963. The have been suppressed. Observers who wish may use format is the same except for some minor changes the omitted symbols of Blagg and Miiller without to improve clarity and legibility. The information in fear of ambiguity. the text of Comm. LPL No. 30 therefore applies to The photographic coverage of the second quad- this Communication also. rant is by no means uniform in quality, and certain Some of the minor changes mentioned above phases are not well represented. Thus for small cra- have been introduced because of the particular ters in certain longitudes there are no good determi- nature of the second lunar quadrant, most of which nations of the diameters, and our values are little is covered by the dark areas Mare Imbrium and better than rough estimates.
    [Show full text]
  • Glossary Glossary
    Glossary Glossary Albedo A measure of an object’s reflectivity. A pure white reflecting surface has an albedo of 1.0 (100%). A pitch-black, nonreflecting surface has an albedo of 0.0. The Moon is a fairly dark object with a combined albedo of 0.07 (reflecting 7% of the sunlight that falls upon it). The albedo range of the lunar maria is between 0.05 and 0.08. The brighter highlands have an albedo range from 0.09 to 0.15. Anorthosite Rocks rich in the mineral feldspar, making up much of the Moon’s bright highland regions. Aperture The diameter of a telescope’s objective lens or primary mirror. Apogee The point in the Moon’s orbit where it is furthest from the Earth. At apogee, the Moon can reach a maximum distance of 406,700 km from the Earth. Apollo The manned lunar program of the United States. Between July 1969 and December 1972, six Apollo missions landed on the Moon, allowing a total of 12 astronauts to explore its surface. Asteroid A minor planet. A large solid body of rock in orbit around the Sun. Banded crater A crater that displays dusky linear tracts on its inner walls and/or floor. 250 Basalt A dark, fine-grained volcanic rock, low in silicon, with a low viscosity. Basaltic material fills many of the Moon’s major basins, especially on the near side. Glossary Basin A very large circular impact structure (usually comprising multiple concentric rings) that usually displays some degree of flooding with lava. The largest and most conspicuous lava- flooded basins on the Moon are found on the near side, and most are filled to their outer edges with mare basalts.
    [Show full text]
  • Chance, Luck and Statistics : the Science of Chance
    University of Calgary PRISM: University of Calgary's Digital Repository Alberta Gambling Research Institute Alberta Gambling Research Institute 1963 Chance, luck and statistics : the science of chance Levinson, Horace C. Dover Publications, Inc. http://hdl.handle.net/1880/41334 book Downloaded from PRISM: https://prism.ucalgary.ca Chance, Luck and Statistics THE SCIENCE OF CHANCE (formerly titled: The Science of Chance) BY Horace C. Levinson, Ph. D. Dover Publications, Inc., New York Copyright @ 1939, 1950, 1963 by Horace C. Levinson All rights reserved under Pan American and International Copyright Conventions. Published in Canada by General Publishing Company, Ltd., 30 Lesmill Road, Don Mills, Toronto, Ontario. Published in the United Kingdom by Constable and Company, Ltd., 10 Orange Street, London, W.C. 2. This new Dover edition, first published in 1963. is a revised and enlarged version ot the work pub- lished by Rinehart & Company in 1950 under the former title: The Science of Chance. The first edi- tion of this work, published in 1939, was called Your Chance to Win. International Standard Rook Number: 0-486-21007-3 Libraiy of Congress Catalog Card Number: 63-3453 Manufactured in the United States of America Dover Publications, Inc. 180 Varick Street New York, N.Y. 10014 PREFACE TO DOVER EDITION THE present edition is essentially unchanged from that of 1950. There are only a few revisions that call for comment. On the other hand, the edition of 1950 contained far more extensive revisions of the first edition, which appeared in 1939 under the title Your Chance to Win. One major revision was required by the appearance in 1953 of a very important work, a life of Cardan,* a brief account of whom is given in Chapter 11.
    [Show full text]
  • Metallicities of the Β Cephei Stars from Low-Resolution Ultraviolet Spectra
    A&A 433, 659–669 (2005) Astronomy DOI: 10.1051/0004-6361:20040396 & c ESO 2005 Astrophysics Metallicities of the β Cephei stars from low-resolution ultraviolet spectra E. Niemczura and J. Daszynska-Daszkiewicz´ Astronomical Institute, Wrocław University, ul. Kopernika 11, 51-622 Wrocław, Poland e-mail: [email protected] Received 5 March 2004 / Accepted 22 November 2004 Abstract. We derive basic stellar parameters (angular diameters, effective temperatures, metallicities) and interstellar reddening for all β Cephei stars observed during the IUE satellite mission, including those belonging to three open clusters. The parameters are derived by means of an algorithmic procedure of fitting theoretical flux distributions to the low-resolution IUE spectra and ground-based spectrophotometric observations. Since the metallicity has a special importance for pulsating B-type stars, we focus our attention in particular on this parameter. Key words. stars: early-type – stars: abundances – stars: variables: general 1. Introduction In this paper we analyze the IUE (International Ultraviolet Explorer) data combined with ground-based spectrophotomet- β Cephei variables are a well-known group of early B-type ric observations of β Cephei stars. The ultraviolet (UV) part pulsating stars. Their pulsations are driven by the classical of the spectra of main-sequence B-type stars is very rich in κ-mechanism, operating in the layer of the metal opacity bump lines of the iron-group elements. Because the greatest amount ≈ × 5 at T 2 10 K caused by the large number of absorption of energy for these objects is emitted in the spectral region be- lines of the iron-group elements.
    [Show full text]
  • The High Energy Astrophysics Division Newsletter
    SPRING 2017 The High Energy Astrophysics Division Newsletter In this Issue: View from the Chair — special advertising section — hidden black holes revealed, and others — second running — finding a path through spacetime — announcing mysteries under the ice — performance enhancements for Chandra — milestones for XMM — the hunt continues for Swift — ULXNS — on the trail of the wild neutrino with INTEGRAL — searching at home with Fermi — energetic electrons seen at the ISS — news from the cosmos — of scientific interest — a Universe of learning — NICER launch prep — SRG progress — the wisdom of Athena — the slant on IXPE — the XARM — building CTA — all-seeing Lynx — in memoriam From the Chair for the discovery of merging black hole binaries, and for beginning the new era of gravitational-wave astronomy. CHRIS REYNOLDS (U. MD) Prof. González will give the Rossi Prize Lecture at the All systems are go for our 16th Divisional meeting to 231st AAS meeting to be held at National Harbor, MD be held in Sun Valley, Idaho, 20-24 August 2017! Regis- in January 2018. Please join me in congratulating all of tration and abstract submission is now open and we’re this year’s HEAD prize winners. looking forward to an exciting scientific program cover- ing all aspects of high-energy astrophysics, kicked off by The past few months has been eventful in the world a total solar eclipse! of high-energy astrophysics missions. NICER and ISS- CREAM are at the Kennedy Space Center and ready for One of the most important aspects of these meet- launch to the International Space Station. Further in the ings is the chance to honor a new batch of HEAD future, NASA has formally selected the Imaging X-ray Po- prize winners.
    [Show full text]
  • The Ohio State University Astronomy Department Columbus, Ohio 43210
    The Ohio State University Astronomy Department Columbus, Ohio 43210 Abstract Zheng Zheng. Justin Oelgoetz is an OSU Chemical This annual report covers the period 2002 September Physics graduate student working on his Ph.D. thesis through 2003 August. with Pradhan. The Masters Degree was awarded to Fields, Mar- 1 PERSONNEL shall, and Onken. During the period covered by this report, the regu- Osmer represents OSU on the Board of Directors lar academic staff of the Department of Astronomy in- of the Large Binocular Telescope Corporation. He is cluded Richard Boyd, Darren DePoy, Jay Frogel, An- a member of the Publications Board of the American drew Gould, Eric Herbst, Smita Mathur, Jordi Miralda- Astronomical Society and also serves on the Board of Escud´e, Gerald Newsom, Patrick Osmer (chairperson), Directors of Research Corporation. Bradley Peterson, Marc Pinsonneault, Richard Pogge, Peterson completed a term as a member of the NASA Anil Pradhan, Barbara Ryden, Robert Scherrer, Kris- Structure and Evolution of the Universe Subcommittee. ten Sellgren, Gary Steigman, Donald Terndrup, Terrance He continues to serve as a member of the Astronomy Walker, and David Weinberg. In addition, Christopher and Astrophysics Advisory Committee (AAAC), which Kochanek has been appointed Ohio Eminent Scholar in was established by Congress to facilitate greater coop- the Department of Astronomy, starting October 1, 2003. eration between the National Science Foundation and Boyd was on leave, serving in the Physics Division of NASA. Peterson is OSU’s institutional representative to the National Science Foundation in Washington, D.C. the AURA Board and this year he was elected to the as Program Director for Nuclear Physics and for Par- Space Telescope Institute Council (STIC).
    [Show full text]
  • Constraints on the Timescale of Animal Evolutionary History
    Palaeontologia Electronica palaeo-electronica.org Constraints on the timescale of animal evolutionary history Michael J. Benton, Philip C.J. Donoghue, Robert J. Asher, Matt Friedman, Thomas J. Near, and Jakob Vinther ABSTRACT Dating the tree of life is a core endeavor in evolutionary biology. Rates of evolution are fundamental to nearly every evolutionary model and process. Rates need dates. There is much debate on the most appropriate and reasonable ways in which to date the tree of life, and recent work has highlighted some confusions and complexities that can be avoided. Whether phylogenetic trees are dated after they have been estab- lished, or as part of the process of tree finding, practitioners need to know which cali- brations to use. We emphasize the importance of identifying crown (not stem) fossils, levels of confidence in their attribution to the crown, current chronostratigraphic preci- sion, the primacy of the host geological formation and asymmetric confidence intervals. Here we present calibrations for 88 key nodes across the phylogeny of animals, rang- ing from the root of Metazoa to the last common ancestor of Homo sapiens. Close attention to detail is constantly required: for example, the classic bird-mammal date (base of crown Amniota) has often been given as 310-315 Ma; the 2014 international time scale indicates a minimum age of 318 Ma. Michael J. Benton. School of Earth Sciences, University of Bristol, Bristol, BS8 1RJ, U.K. [email protected] Philip C.J. Donoghue. School of Earth Sciences, University of Bristol, Bristol, BS8 1RJ, U.K. [email protected] Robert J.
    [Show full text]
  • On the Detection of Exoplanets Via Radial Velocity Doppler Spectroscopy
    The Downtown Review Volume 1 Issue 1 Article 6 January 2015 On the Detection of Exoplanets via Radial Velocity Doppler Spectroscopy Joseph P. Glaser Cleveland State University Follow this and additional works at: https://engagedscholarship.csuohio.edu/tdr Part of the Astrophysics and Astronomy Commons How does access to this work benefit ou?y Let us know! Recommended Citation Glaser, Joseph P.. "On the Detection of Exoplanets via Radial Velocity Doppler Spectroscopy." The Downtown Review. Vol. 1. Iss. 1 (2015) . Available at: https://engagedscholarship.csuohio.edu/tdr/vol1/iss1/6 This Article is brought to you for free and open access by the Student Scholarship at EngagedScholarship@CSU. It has been accepted for inclusion in The Downtown Review by an authorized editor of EngagedScholarship@CSU. For more information, please contact [email protected]. Glaser: Detection of Exoplanets 1 Introduction to Exoplanets For centuries, some of humanity’s greatest minds have pondered over the possibility of other worlds orbiting the uncountable number of stars that exist in the visible universe. The seeds for eventual scientific speculation on the possibility of these "exoplanets" began with the works of a 16th century philosopher, Giordano Bruno. In his modernly celebrated work, On the Infinite Universe & Worlds, Bruno states: "This space we declare to be infinite (...) In it are an infinity of worlds of the same kind as our own." By the time of the European Scientific Revolution, Isaac Newton grew fond of the idea and wrote in his Principia: "If the fixed stars are the centers of similar systems [when compared to the solar system], they will all be constructed according to a similar design and subject to the dominion of One." Due to limitations on observational equipment, the field of exoplanetary systems existed primarily in theory until the late 1980s.
    [Show full text]
  • Exploration of Mars by the European Space Agency 1
    Exploration of Mars by the European Space Agency Alejandro Cardesín ESA Science Operations Mars Express, ExoMars 2016 IAC Winter School, November 20161 Credit: MEX/HRSC History of Missions to Mars Mars Exploration nowadays… 2000‐2010 2011 2013/14 2016 2018 2020 future … Mars Express MAVEN (ESA) TGO Future ESA (ESA- Studies… RUSSIA) Odyssey MRO Mars Phobos- Sample Grunt Return? (RUSSIA) MOM Schiaparelli ExoMars 2020 Phoenix (ESA-RUSSIA) Opportunity MSL Curiosity Mars Insight 2020 Spirit The data/information contained herein has been reviewed and approved for release by JPL Export Administration on the basis that this document contains no export‐controlled information. Mars Express 2003-2016 … First European Mission to orbit another Planet! First mission of the “Rosetta family” Up and running since 2003 Credit: MEX/HRSC First European Mission to orbit another Planet First European attempt to land on another Planet Original mission concept Credit: MEX/HRSC December 2003: Mars Express Lander Release and Orbit Insertion Collission trajectory Bye bye Beagle 2! Last picture Lander after release, release taken by VMC camera Insertion 19/12/2003 8:33 trajectory Credit: MEX/HRSC Beagle 2 was found in January 2015 ! Only 6km away from landing site OK Open petals indicate soft landing OK Antenna remained covered Lessons learned: comms at all time! Credit: MEX/HRSC Mars Express: so many missions at once Mars Mission Phobos Mission Relay Mission Credit: MEX/HRSC Mars Express science investigations Martian Moons: Phobos & Deimos: Ionosphere, surface,
    [Show full text]
  • Mars Exploration - a Story Fifty Years Long Giuseppe Pezzella and Antonio Viviani
    Chapter Introductory Chapter: Mars Exploration - A Story Fifty Years Long Giuseppe Pezzella and Antonio Viviani 1. Introduction Mars has been a goal of exploration programs of the most important space agencies all over the world for decades. It is, in fact, the most investigated celestial body of the Solar System. Mars robotic exploration began in the 1960s of the twentieth century by means of several space probes sent by the United States (US) and the Soviet Union (USSR). In the recent past, also European, Japanese, and Indian spacecrafts reached Mars; while other countries, such as China and the United Arab Emirates, aim to send spacecraft toward the red planet in the next future. 1.1 Exploration aims The high number of mission explorations to Mars clearly points out the impor- tance of Mars within the Solar System. Thus, the question is: “Why this great interest in Mars exploration?” The interest in Mars is due to several practical, scientific, and strategic reasons. In the practical sense, Mars is the most accessible planet in the Solar System [1]. It is the second closest planet to Earth, besides Venus, averaging about 360 million kilometers apart between the furthest and closest points in its orbit. Earth and Mars feature great similarities. For instance, both planets rotate on an axis with quite the same rotation velocity and tilt angle. The length of a day on Earth is 24 h, while slightly longer on Mars at 24 h and 37 min. The tilt of Earth axis is 23.5 deg, and Mars tilts slightly more at 25.2 deg [2].
    [Show full text]
  • Sulfur Hazes in Giant Exoplanet Atmospheres: Impacts on Reflected
    Draft version February 28, 2017 Preprint typeset using LATEX style AASTeX6 v. 1.0 SULFUR HAZES IN GIANT EXOPLANET ATMOSPHERES: IMPACTS ON REFLECTED LIGHT SPECTRA Peter Gao1,2,3, Mark S. Marley, and Kevin Zahnle NASA Ames Research Center Moffett Field, CA 94035, USA Tyler D. Robinson4,5 Department of Astronomy and Astrophysics University of California Santa Cruz Santa Cruz, CA 95064, USA Nikole K. Lewis Space Telescope Science Institute Baltimore, MD 21218, USA 1Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 2NASA Postdoctoral Program Fellow [email protected] 4Sagan Fellow 5NASA Astrobiology Institute’s Virtual Planetary Laboratory ABSTRACT Recent work has shown that sulfur hazes may arise in the atmospheres of some giant exoplanets due to the photolysis of H2S. We investigate the impact such a haze would have on an exoplanet’s geometric albedo spectrum and how it may affect the direct imaging results of WFIRST, a planned NASA space telescope. For temperate (250 K < Teq < 700 K) Jupiter–mass planets, photochemical destruction of H2S results in the production of 1 ppmv of S8 between 100 and 0.1 mbar, which, if cool enough, ∼ will condense to form a haze. Nominal haze masses are found to drastically alter a planet’s geometric albedo spectrum: whereas a clear atmosphere is dark at wavelengths between 0.5 and 1 µm due to molecular absorption, the addition of a sulfur haze boosts the albedo there to 0.7 due to scattering. ∼ Strong absorption by the haze shortward of 0.4 µm results in albedos <0.1, in contrast to the high albedos produced by Rayleigh scattering in a clear atmosphere.
    [Show full text]