DOCSLIB.ORG

Presenting Authors, Co-Authors Abstract Title Abstract in 150 Words Or Less: Institution Z. Brown*, T. Koskinen, I. Müller

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Presenting Authors, Co-Authors Abstract Title Abstract in 150 Words Or Less: Institution Z. Brown*, T. Koskinen, I. Müller Presenting authors, co-authors Abstract Title Abstract in 150 words or less: Institution Z. Brown*, T. Koskinen, I. Müller- A 2D Snapshot of Saturn's Upper Stellar occultations by orbiting spacecraft probe the upper atmospheres of solar University of Arizona Lunar and Wodarg, R. West, A. Jouchoux, L. Atmosphere from Cassini Grand Finale system planets, making them crucial analogs for exoplanets, which cannot be Planetary Laboratory Esposito *presenting author Stellar Occultations explored in the same level of detail. The Cassini Ultraviolet Imaging Spectrograph (UVIS) observed UV-bright O, A, and B stars as they passed behind the limb of Saturn, allowing for profiles of density and temperature in the upper atmosphere. By analyzing UVIS stellar occultations from 2016 and 2017, including Grand Finale data, we created the first 2D maps of Saturn’s density and temperature in thermosphere, from which we infer horizontal winds. Our results have implications the "energy-crisis" of the outer planet thermospheres, which are hotter than can be explained by solar heating alone. Our results indicate that Joule heating at auroral latitudes is important and that this energy can be transported to lower latitudes, adding to growing evidence that this mechanism contributes significantly to the observed temperatures. Chenliang Huang Tommi Koskinen A hydrodynamic study of radiative cooling The heating by photo-ionization in the thermosphere of short-period University of Arizona and escape of metal species in hot Jupiter exoplanets can drive hydrodynamic escape, which is key to understanding the atmospheres evolution of the planet atmosphere and explaining the atmospheric measurements. Besides powering the atmosphere escape, the energy deposited by EUV photons from the host star can also be radiated away through collisional excited atomic spectral lines, leading the mass loss rate to fall significantly below the energy limit. Recent observations have detected evidence of atomic Mg and Fe absorptions in the NUV transmission spectrum of hot Jupiter WASP-121b and HD 209458b. Studying the signature of these atomic lines not only can reveal the structure of the upper atmosphere, but also constrain the radiative cooling rates. In this work, we expand the capability of the exoplanet hydrodynamic atmosphere code of Koskinen et al. (2013) to calculate processes of atomic metal species and compare the results with available observations. J.T.S. Cahill, A.A. Wirth, K.R. A Near and Far Ultraviolet Examination of Due to lunar space weathering (solar wind and micrometeorite bombardment), JHU Applied Physics Lab Stockstill-Cahil, A. Hendrix, and K. Global Lunar Regolith the lunar surface matures producing submicroscopic iron which becomes Retherford encased in impact melt rinds and coats regolith grains. This process manifests differently depending upon the region of the electromagnetic spectrum examined [1, 2]. LRO Lyman Alpha Mapping Project and the Lunar Reconnaissance Orbiter Camera (LROC) Wide Angle Camera (WAC) offer the ability to further assess and characterize this possibility, recording global observations of the lunar regolith between the far- to near-ultraviolet (80 to 690 nm). LROC’s WAC offers a daytime perspective of the Moon in bidirectional reflectance with multiple viewing geometries, while LAMP offers the ability to observe the lunar regolith during both the nighttime and daytime. Here, we leverage these perspectives to further examine any latitudinal variations in regolith maturation. [1] Hendrix et al. (2012) JGR, 117. [2] Hemingway et al. (2015) Icarus, 261, 66. Keri Hoadley (presenter), A one-of-a-kind UV nebula reveals an We report the discovery of the only ultraviolet-emitting planetary nebula-like caltech.edu Christopher Martin, Brian Metzger, ancient merger object discovered to date, which we call the Blue Ring Nebula (BRN). The BRN Mark Seibert, J. Don Neill, Andy was discovered during the GALEX FUV/NUV Deep Imaging Survey in 2004. Since McWilliam, and Ken Shen then, a multi-wavelength investigation, expanding to wavelengths visible from the ground (visible to near-IR photometry, spectroscopy, and time-series data sets), has been made in an attempt to understand the nature and origin of this unique nebula. I will report on the characteristics of the Blue Ring Nebula, what best explains it, and what ground-based observations and results tell us about this nebula’s possible origins. I will also talk about how future UV observations are key to answering many of the open questions remaining about the origins and evolution of this object, as well as understand if it is a truly unique object. Michael W. Davis Alice and UVS: A Quarter Century of Far UV Four compact planetary ultraviolet spectrographs have been built by Southwest Southwest Research Institute Spectrographs Research Institute and successfully operated on different planetary missions: Rosetta-Alice, New Horizons-Alice, LRO-LAMP, and Juno-UVS. A fifth UVS was recently delivered for ESA’s JUICE mission to the moons of Jupiter. A sixth UVS is under construction for the Europa Clipper mis-sion. All of these spectrographs operate in a spectral range encompassed by 50-210 nm. The evolution of the opto-mechanical design will be discussed, along with improvements in detector performance. Lessons learned from integration and test at both the instrument build and spacecraft level will be revealed, including how to stimulate the instrument with FUV light while in an ambient (non-vacuum) environment. Finally, contamination control theory, implemen-tation, and results from five flight UV spectrograph builds will be examined. Leonardo dos Santos (presenting), Atmospheric escape in Neptune-sized and High-energy irradiation (X-rays to ultraviolet) are the main drivers for University of Geneva David Ehrenreich, Vincent Bourrier smaller exoplanets atmospheric escape in short period exoplanets. Since the detection of hydrogen and metals escaping the atmospheres of hot Jupiters, multiple results have surfaced showing that Neptune-sized planets are strongly susceptible to photoevaporation due to vigorous atmospheric loss. Both large-scale populational studies and intensive single-object studies are crucial to understand the role of atmospheric escape in exoplanets. In this contribution, I will briefly review the most recent intensive campaigns to study the high-energy environment and escape in Neptune-sized and smaller planets, such as GJ 436 b, HAT-P-11 b, K2-18 b, and the TRAPPIST-1 system. I will also briefly discuss the potential avenues for future intensive observational campaigns using space- and ground-based facilities that will help us better understand atmospheric escape and evolution in this class of planets. Asa G. Stahl Christopher M. Johns- Candidate Detection of a Hot Jupiter Around We have detected a candidate 2.2 M_Jup planet around a disk-hosting star in Rice University Krull a Disked Star Upper Scorpius, which, if confirmed, would offer a powerful window into how hot Jupiters form and present an exceptional case study for theories of migration. If verified, this would be the second robust detection of a planet embedded in a disk, the first detection of a young hot Jupiter with e > 0.6, and the second potential detection of a hot Jupiter undergoing destructive migration. Corrales, L., Ravi, S., Holguin, F., Capturing exoplanet transits with Swift- Transmission spectroscopy – the direct characterization of exoplanet University of Michigan May, E., Rauscher, E., Reynolds, M. UVOT atmospheres through multi-wavelength observations of exoplanet transits – is newly being explored at wavelengths shorter than optical. Repurposing high energy missions, new research has demonstrated that X-ray and UV observations of exoplanet transits is possible and can reveal signatures of atmospheric evaporation. We will give preliminary results for five hot Jupiters transits observed with the UVOT instrument on the Neil Gehrels Swift Observatory. Finally, we will discuss what UV signatures of exoplanet atmospheres might reveal about atmospheric composition. James Paul Mason, Meng Jin, Kevin Coronal Dimming, Mass Ejections, and the When coronal mass ejections depart the corona, they leave behind a transient University of Colorado, Boulder France, ESCAPE Team ESCAPE SMEX Mission void. Such a region of evacuated plasma is known as a coronal dimming and it contains information about the kinematics of the CME that produced it: dimming slope proportional to CME speed, dimming depth proportional to CME mass. Dimming is so great that it reduces the total energy output of the star in particular emission lines, i.e., dimming is observable in irradiance. We use the Solar Dynamics Observatory (SDO) EUV Variability Experiment (EVE) to parameterize 13 million light curves for dimming. We present this series of dimming studies along with supporting MHD simulations. Finally, we overview the ESCAPE SMEX mission, which will produce SDO/EVE-like measurements for other stars. Among other science objectives, it will (likely) be the first astrophysics mission capable of detecting stellar dimming, which we will use to determine stellar CME kinematics. Arika Egan CUTE: Moving Towards Flight Readiness and The Colorado Ultraviolet Transit Experiment (CUTE) will be the first space Laboratory for Atmospheric and Space Atmospheric Characterization mission launched exclusively for the characterization of exoplanetary Physics atmospheres. Scheduled to fly in March 2021, CUTE is a 6U CubeSat that will spend its nominal 8-month
Load more

Recommended publications
  • Key and Driving Requirements for the Juno Payload Suite of Instruments
    Key and Driving Requirements for the Juno Payload Suite of Instruments Randy Dodge1 and Mark A. Boyles2 Jet Propulsion Laboratory-California Institute of Technology, Pasadena, CA, 91109-8099 Chuck E. Rasbach3 Lockheed Martin-Space System Company, Denver, CO, 80201 [Abstract] The Juno Mission was selected in the summer of 2005 via NASA’s New Frontiers competitive AO process (refer to http://www.nasa.gov/home/hqnews/2005/jun/HQ_05138_New_Frontiers_2.html). The Juno project is led by a Principle Investigator based at Southwest Research Institute [SwRI] in San Antonio, Texas, with project management based at the Jet Propulsion Laboratory [JPL] in Pasadena, California, while the Spacecraft design and Flight System integration are under contract to Lockheed Martin Space Systems Company [LM-SSC] in Denver, Colorado. The payload suite consists of a large number of instruments covering a wide spectrum of experimentation. The science team includes a lead Co-Investigator for each one of the following experiments: A Magnetometer experiment (consisting of both a FluxGate Magnetometer (FGM) built at Goddard Space Flight Center [GSFC] and a Scalar Helium Magnetometer (SHM) built at JPL, a MicroWave Radiometer (MWR) also built at JPL, a Gravity Science experiment (GS) implemented via the telecom subsystem, two complementary particle instruments (Jovian Auroral Distribution Experiment, JADE developed by SwRI and Juno Energetic-particle Detector Instrument, JEDI from the Applied Physics Lab [APL]--JEDI and JADE both measure electrons and ions), an Ultraviolet Spectrometer (UVS) also developed at SwRI, and a radio and plasma (Waves) experiment (from the University of Iowa). In addition, a visible camera (JunoCam) is included in the payload to facilitate education and public outreach (designed & fabricated by Malin Space Science Systems [MSSS]).
    [Show full text]
  • JUICE Red Book
    ESA/SRE(2014)1 September 2014 JUICE JUpiter ICy moons Explorer Exploring the emergence of habitable worlds around gas giants Definition Study Report European Space Agency 1 This page left intentionally blank 2 Mission Description Jupiter Icy Moons Explorer Key science goals The emergence of habitable worlds around gas giants Characterise Ganymede, Europa and Callisto as planetary objects and potential habitats Explore the Jupiter system as an archetype for gas giants Payload Ten instruments Laser Altimeter Radio Science Experiment Ice Penetrating Radar Visible-Infrared Hyperspectral Imaging Spectrometer Ultraviolet Imaging Spectrograph Imaging System Magnetometer Particle Package Submillimetre Wave Instrument Radio and Plasma Wave Instrument Overall mission profile 06/2022 - Launch by Ariane-5 ECA + EVEE Cruise 01/2030 - Jupiter orbit insertion Jupiter tour Transfer to Callisto (11 months) Europa phase: 2 Europa and 3 Callisto flybys (1 month) Jupiter High Latitude Phase: 9 Callisto flybys (9 months) Transfer to Ganymede (11 months) 09/2032 – Ganymede orbit insertion Ganymede tour Elliptical and high altitude circular phases (5 months) Low altitude (500 km) circular orbit (4 months) 06/2033 – End of nominal mission Spacecraft 3-axis stabilised Power: solar panels: ~900 W HGA: ~3 m, body fixed X and Ka bands Downlink ≥ 1.4 Gbit/day High Δv capability (2700 m/s) Radiation tolerance: 50 krad at equipment level Dry mass: ~1800 kg Ground TM stations ESTRAC network Key mission drivers Radiation tolerance and technology Power budget and solar arrays challenges Mass budget Responsibilities ESA: manufacturing, launch, operations of the spacecraft and data archiving PI Teams: science payload provision, operations, and data analysis 3 Foreword The JUICE (JUpiter ICy moon Explorer) mission, selected by ESA in May 2012 to be the first large mission within the Cosmic Vision Program 2015–2025, will provide the most comprehensive exploration to date of the Jovian system in all its complexity, with particular emphasis on Ganymede as a planetary body and potential habitat.
    [Show full text]
  • Juno Spacecraft Description
    Juno Spacecraft Description By Bill Kurth 2012-06-01 Juno Spacecraft (ID=JNO) Description The majority of the text in this file was extracted from the Juno Mission Plan Document, S. Stephens, 29 March 2012. [JPL D-35556] Overview For most Juno experiments, data were collected by instruments on the spacecraft then relayed via the orbiter telemetry system to stations of the NASA Deep Space Network (DSN). Radio Science required the DSN for its data acquisition on the ground. The following sections provide an overview, first of the orbiter, then the science instruments, and finally the DSN ground system. Juno launched on 5 August 2011. The spacecraft uses a deltaV-EGA trajectory consisting of a two-part deep space maneuver on 30 August and 14 September 2012 followed by an Earth gravity assist on 9 October 2013 at an altitude of 559 km. Jupiter arrival is on 5 July 2016 using two 53.5-day capture orbits prior to commencing operations for a 1.3-(Earth) year-long prime mission comprising 32 high inclination, high eccentricity orbits of Jupiter. The orbit is polar (90 degree inclination) with a periapsis altitude of 4200-8000 km and a semi-major axis of 23.4 RJ (Jovian radius) giving an orbital period of 13.965 days. The primary science is acquired for approximately 6 hours centered on each periapsis although fields and particles data are acquired at low rates for the remaining apoapsis portion of each orbit. Juno is a spin-stabilized spacecraft equipped for 8 diverse science investigations plus a camera included for education and public outreach.
    [Show full text]
  • Auroral Emission at Jupiter Through Juno's UVS Eyes
    Auroral emission at Jupiter through Juno's UVS eyes Denis Grodent Bertrand Bonfond G. Randy Gladstone Jean-Claude Gérard Jacques Gusn Aikaterini Radio= Maïté Dumont Benjamin Palmaerts the Juno Science Team LPAP, Université de Liège, Belgium Southwest Research InsBtute, USA UVS D. Grodent ULg TheJuno UltravioletUltraViolet Spectrograph on Spectrograph UVS NASA’s Juno Mission (PI: G.R. Gladstone) Fig. 4 An opto-mechanical schematic of the Juno-UVS sensor showing light rays traced through the main apertureGladstone et al. 2014 door, reflecting from the OAP primary, passing through a focus at the slit, diffracted off the toroidal grating, and imaged onto the XDL MCP detector UV light D. Grodent ULg 3.3 Detector and Detector Electronics The Juno-UVS detector configuration includes an XDL microchannel plate (MCP) detector scheme housed in a vacuum enclosure with a one-time opening door containing a UV-grade fused-silica window (for limited UV throughput during testing). The door was spring loaded for opening with a wax-pellet-type push actuator. The vacuum enclosure has a vacuum pump port and a small, highly polished region which functions as a zero-order reflector (directing zero-order light from the instrument grating into the zero-order trap on the side of the in- strument housing). The vacuum enclosure also utilizes four female connectors for the anode signals, and two high-voltage (HV) connectors for the MCP and anode gap voltages. The detector’s MCP configuration uses a Z-stack that is cylindrically curved to match the 150-mm Rowland circle diameter to optimize spectral and spatial focus across the Juno- UVS bandpass.
    [Show full text]
  • Juno Magnetometer (MAG) Standard Product Data Record and Archive Volume Software Interface Specification
    Juno Magnetometer Juno Magnetometer (MAG) Standard Product Data Record and Archive Volume Software Interface Specification Preliminary March 6, 2018 Prepared by: Jack Connerney and Patricia Lawton Juno Magnetometer MAG Standard Product Data Record and Archive Volume Software Interface Specification Preliminary March 6, 2018 Approved: John E. P. Connerney Date MAG Principal Investigator Raymond J. Walker Date PDS PPI Node Manager Concurrence: Patricia J. Lawton Date MAG Ground Data System Staff 2 Table of Contents 1 Introduction ............................................................................................................................. 1 1.1 Distribution list ................................................................................................................... 1 1.2 Document change log ......................................................................................................... 2 1.3 TBD items ........................................................................................................................... 3 1.4 Abbreviations ...................................................................................................................... 4 1.5 Glossary .............................................................................................................................. 6 1.6 Juno Mission Overview ...................................................................................................... 7 1.7 Software Interface Specification Content Overview .........................................................
    [Show full text]
  • Investigations of Moon-Magnetosphere Interactions by the Europa Clipper Mission
    EPSC Abstracts Vol. 13, EPSC-DPS2019-366-1, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. Investigations of Moon-Magnetosphere Interactions by the Europa Clipper Mission Haje Korth (1), Robert T. Pappalardo (2), David A. Senske (2), Sascha Kempf (3), Margaret G. Kivelson (4,5), Kurt Retherford (6), J. Hunter Waite (6), Joseph H. Westlake (1), and the Europa Clipper Science Team (1) Johns Hopkins University Applied Physics Laboratory, Maryland, USA, (2) Jet Propulsion Laboratory, California, USA, (3) University of Colorado, Colorado, USA, (4) University of Michigan, Michigan, USA, (5) University of California, California, USA, (6) Southwest Research Institute, Texas, USA. ([email protected]) 1. Introduction magnetic fields inducing eddy currents in the ocean. By measuring the induced field response at multiple The influence of the Jovian space environment on frequencies, the ice shell thickness and the ocean Europa is multifaceted, and observations of moon- layer thickness and conductivity can be uniquely magnetosphere interaction by the Europa Clipper will determined. The ECM consists of four fluxgate provide an understanding of the satellite’s interior sensors mounted on a 5-m-long boom and a control structure and compositional makeup among others. electronics hosted in a vault shielding it from The variability of Jupiter’s magnetic field at Europa radiation damage. The use of four sensors allows for induces electric currents within the moon’s dynamic removal of higher-order spacecraft- conducting ocean layer, the magnitude of which generated magnetic fields on a boom that is short depends on the ocean’s location, extent, and compared with the spacecraft dimensions.
    [Show full text]
  • PPS01-P08 Japan Geoscience Union Meeting 2016
    PPS01-P08 Japan Geoscience Union Meeting 2016 Statistical study of the response of Jovian EUV aurora to the solar wind from Hisaki observations Hajime Kita1, Tomoki Kimura2, Chihiro Tao3, *Fuminori Tsuchiya1, Hiroaki Misawa1, Takeshi Sakanoi1, Yasumasa Kasaba1, Go Murakami4, Kazuo Yoshioka5, Atsushi Yamazaki4, Ichiro Yoshikawa6 1.Graduate School of Science, Tohoku University, 2.Nishina-Center for Accelerator Based Science, RIKEN, 3.National Institute of Information and Communications Technology, 4.Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 5.Department of Earth and Planetary Science, Graduate School of Science, University of Tokyo, 6.Department of Complexity Science and Engineering, University of Tokyo In order to reveal the solar wind response of Jovian extreme ultraviolet (EUV) auroral activity, we made a statistical analysis of Jovian EUV aurora obtained from long term Hisaki observation. The EUV emission from hydrogen molecule is excited by collision with high energy electron. The main oval is one of the components of Jovian EUV aurora where the auroral particle precipitations are caused by the rotationally driven field-aligned current system. It is theoretically expected that angular velocity of magnetospheric plasma increases when the Jovian magnetosphere is compressed by enhanced solar wind pressure, which decreases the field-aligned current. Regarding this scenario, increase of the solar wind dynamic pressure is expected to be anti-correlated with the intensity of the EUV aurora. A previous observation such as that by International Ultraviolet Explorer (IUE) or Hubble Space Telescope (HST) showed the time variability of the EUV aurora, while their data still limited in continuity over solar wind variation with good time resolution.
    [Show full text]
  • Cosmic Evolution Through Uv Surveys (Cetus) Final Report
    COSMIC EVOLUTION THROUGH UV SURVEYS (CETUS) FINAL REPORT Thematic Activity: Project (probe mission concept) Program: Electromagnetic observations from space Authors of Final Report: Jonathan Arenberg, Northrop Grumman Corporation Sally Heap, Univ. of Maryland, [email protected] Tony Hull, Univ. of New Mexico Steve Kendrick, Kendrick Aerospace Consulting LLC Bob Woodruff, Woodruff Consulting Scientific Contributors: Maarten Baes, Rachel Bezanson, Luciana Bianchi, David Bowen, Brad Cenko, Yi-Kuan Chiang, Rachel Cochrane, Mike Corcoran, Paul Crowther, Simon Driver, Bill Danchi, Eli Dwek, Brian Fleming, Kevin France, Pradip Gatkine, Suvi Gezari, Lea Hagen, Chris Hayward, Matthew Hayes, Tim Heckman, Edmund Hodges-Kluck, Alexander Kutyrev, Thierry Lanz, John MacKenty, Steve McCandliss, Harvey Moseley, Coralie Neiner, Goren Östlin, Camilla Pacifici, Marc Rafelski, Bernie Rauscher, Jane Rigby, Ian Roederer, David Spergel, Dan Stark, Alexander Szalay, Bryan Terrazas, Jonathan Trump, Arjun van der Wel, Sylvain Veilleux, Kate Whitaker, Isak Wold, Rosemary Wyse Technical Contributors: Jim Burge, Kelly Dodson, Chip Eckles, Brian Fleming, Jamie Kennea, Gerry Lemson, John MacKenty, Steve McCandliss, Greg Mehle, Shouleh Nikzad, Trent Newswander, Lloyd Purves, Manuel Quijada, Ossy Siegmund, Dave Sheikh, Phil Stahl, Ani Thakar, John Vallerga, Marty Valente, the Goddard IDC/MDL. September 2019 Cosmic Evolution Through UV Surveys (CETUS) TABLE OF CONTENTS INTRODUCTION TO CETUS ................................................................................................................
    [Show full text]
  • Dr. Renyu Hu August 12, 2021
    Dr. Renyu Hu August 12, 2021 Jet Propulsion Laboratory 1 (818) 281 9459 4800 Oak Grove Dr., MS 169-237 [email protected] Pasadena, CA 91109, USA http://web.gps.caltech.edu/~ryh/ EMPLOYMENT 2019- Scientist IV, Jet Propulsion Laboratory 2015-19 Scientist III, Jet Propulsion Laboratory 2013-15 Hubble Fellow, Jet Propulsion Laboratory EDUCATION 2013 Ph.D., Planetary Sciences, Massachusetts Institute of Technology “Atmospheric Photochemistry, Surface Features, and Potential Biosignature Gases of Terrestrial Exoplanets,” Advisor: Sara Seager 2009 M.S., Astrophysics, Tsinghua University 2009 Diplôme d'Ingénieur (French Engineer’s Degree), École Centrale Paris 2007 B.S., Mathematics and Physics, Tsinghua University FIELDS OF INTEREST Atmospheres of planets and exoplanets from Earth-sized to Jupiter-sized. Remote sensing of planets using transit spectroscopy, phase curve mapping, and direct imaging. Evolution of planetary atmospheres and stable isotope geochemistry. Search for habitable planets and biosignatures. Gas and aqueous phase chemical kinetics. SELECTED AWARDS AND HONORS 2021 JPL Edward Stone Award for Outstanding Research Publication 2020 NASA Early Career Public Achievement Medal 2019 NASA Group Achievement Award for the Astrophysics Large Mission Studies 2017 JPL Voyager Award for Individual Achievement 2013-15 NASA Hubble Fellowship 2011-13 NASA Earth and Space Science Fellowship 2012 Barrett Prize, Massachusetts Institute of Technology 2011 Fellowship, NASA Astrobiology Institute Summer School 2009 Presidential Fellowship, Massachusetts
    [Show full text]
  • 2019 Astrophysics Senior Review Senior Review Subcommittee Report
    2019 Astrophysics Senior Review Senior Review Subcommittee Report 2019 Astrophysics Senior Review - Senior Review Subcommittee Report June 4-5, 2019 SUBCOMMITTEE MEMBERS Dr. Alison Coil, University of California San Diego Dr. Megan Donahue, Michigan State University Dr. Jonathan Fortney, University of California Santa Cruz Ms. Maura Fujieh, NASA Ames Research Center Dr. Roberta Humphreys, University of Minnesota Dr. Mark McConnell, University of New Hampshire / Southwest Research Institute Dr. John O’Meara, Keck Observatory Dr. Rebecca Oppenheimer, American Museum of Natural History Dr. Alexandra Pope, University of Massachusetts Amherst Dr. Wilton Sanders, NASA/University of Wisconsin-Madison, retired Dr. David Weinberg, The Ohio State University - Chair ​ 1 EXECUTIVE SUMMARY The eight missions evaluated by the 2019 Astrophysics Senior Review constitute a portfolio of extraordinary scientific power, on topics that range from the atmospheres of planets around nearby stars to the nature of the dark energy that drives the accelerating expansion of the cosmos. The missions themselves range from the venerable Great Observatories Hubble and Chandra to the newest Explorer missions NICER and TESS. ​ ​ ​ ​ ​ All of these missions are operating at a high level technically and scientifically, and all have sought ways to make their operations cost-efficient and their data valuable to a broad community. The complementary nature of these missions makes the overall capability of the portfolio more than the sum of its parts, and many of the most exciting developments in contemporary astrophysics draw on observations from several of these observatories simultaneously. The Senior Review Subcommittee recommends that NASA continue to operate and support all eight of these missions.
    [Show full text]
  • Securing Japan an Assessment of Japan´S Strategy for Space
    Full Report Securing Japan An assessment of Japan´s strategy for space Report: Title: “ESPI Report 74 - Securing Japan - Full Report” Published: July 2020 ISSN: 2218-0931 (print) • 2076-6688 (online) Editor and publisher: European Space Policy Institute (ESPI) Schwarzenbergplatz 6 • 1030 Vienna • Austria Phone: +43 1 718 11 18 -0 E-Mail: [email protected] Website: www.espi.or.at Rights reserved - No part of this report may be reproduced or transmitted in any form or for any purpose without permission from ESPI. Citations and extracts to be published by other means are subject to mentioning “ESPI Report 74 - Securing Japan - Full Report, July 2020. All rights reserved” and sample transmission to ESPI before publishing. ESPI is not responsible for any losses, injury or damage caused to any person or property (including under contract, by negligence, product liability or otherwise) whether they may be direct or indirect, special, incidental or consequential, resulting from the information contained in this publication. Design: copylot.at Cover page picture credit: European Space Agency (ESA) TABLE OF CONTENT 1 INTRODUCTION ............................................................................................................................. 1 1.1 Background and rationales ............................................................................................................. 1 1.2 Objectives of the Study ................................................................................................................... 2 1.3 Methodology
    [Show full text]
  • New Year's Address January 4, 2017 Saku Tsuneta, Director General
    New Year’s Address January 4, 2017 Saku Tsuneta, Director General, Institute of Space and Astronautical Science Happy New Year, everyone. I hope most of the staff members of this institute have enjoyed their New Year’s vacation although it was not so long, and I am especially thankful to those people working hard in the critical phase of the Arase mission and those preparing for the launch of SS-520-4, including the support members of manufacturers. Successful launch of Arase and Epsilon launch vehicle In late December, we successfully launched ARASE, or the Exploration of energization and Radiation in Geospace (ERG) satellite, using the Epsilon-2 Launch Vehicle. It was a truly wonderful launch experience for all of us. The Epsilon launch vehicle was developed and launched under the management of the Space Technology Directorate I of JAXA. Hence, the Project Manager, Dr. Yasuhiro Morita led the overall program management and Mr. Takayuki Imoto acted as the sub-manager to command the frontline. I would like to say special thanks to both leaders and the project members of JAXA and ISAS who have been involved in this program. The second-stage rocket of Epsilon-2 has been newly developed to give it higher performance and a lower cost, and the launch capability has increased by about 30 percent from that of Epsilon-1. These newly developed technologies will be used in the solid rocket booster, SRB-3, of the H3 launch vehicle. Then, the SRB-3 booster will be used as the first-stage rocket of Epsilon launch vehicles.
    [Show full text]