Full-Sun Observations for Identifying the Source of the Slow Solar Wind
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Astronomy & Astrophysics a Hipparcos Study of the Hyades
A&A 367, 111–147 (2001) Astronomy DOI: 10.1051/0004-6361:20000410 & c ESO 2001 Astrophysics A Hipparcos study of the Hyades open cluster Improved colour-absolute magnitude and Hertzsprung{Russell diagrams J. H. J. de Bruijne, R. Hoogerwerf, and P. T. de Zeeuw Sterrewacht Leiden, Postbus 9513, 2300 RA Leiden, The Netherlands Received 13 June 2000 / Accepted 24 November 2000 Abstract. Hipparcos parallaxes fix distances to individual stars in the Hyades cluster with an accuracy of ∼6per- cent. We use the Hipparcos proper motions, which have a larger relative precision than the trigonometric paral- laxes, to derive ∼3 times more precise distance estimates, by assuming that all members share the same space motion. An investigation of the available kinematic data confirms that the Hyades velocity field does not contain significant structure in the form of rotation and/or shear, but is fully consistent with a common space motion plus a (one-dimensional) internal velocity dispersion of ∼0.30 km s−1. The improved parallaxes as a set are statistically consistent with the Hipparcos parallaxes. The maximum expected systematic error in the proper motion-based parallaxes for stars in the outer regions of the cluster (i.e., beyond ∼2 tidal radii ∼20 pc) is ∼<0.30 mas. The new parallaxes confirm that the Hipparcos measurements are correlated on small angular scales, consistent with the limits specified in the Hipparcos Catalogue, though with significantly smaller “amplitudes” than claimed by Narayanan & Gould. We use the Tycho–2 long time-baseline astrometric catalogue to derive a set of independent proper motion-based parallaxes for the Hipparcos members. -
Hinode Project and Science Center (Hinode-SC)
Hinode Project and Science Center (Hinode-SC) Shinsuke Imada (Nagoya Univ., ISEE) Characteristics of the Advanced Telescopes | Hinode Science Center at NAOJ 2019/10/13 22(30 For Researchers 日本語 シェア Tweet “Hinode” Unveils To do research Information Gallery For Researchers the Mysteries of the Sun using Hinode data TOP "Hinode" Unveils the Mysteries of the Sun Characteristics of the Advanced Telescopes Solar Observing Satellite "Hinode" (SOLAR-B) | Hinode Science Center at NAOJ 2019/10/13 22(29 "Hinode" Unveils Characteristics of the Advanced Telescopes the Mysteries of the For Researchers 日本語 Sun Tweet シェア Overview of “Hinode” “Hinode” Unveils To do research Characteristics of the Advanced Telescopes Solar Observing Information Gallery For Researchers Satellite "Hinode" the Mysteries of the Sun using Hinode data (SOLAR-B) The Sun's atmosphere is comprised of layers. The layers beneath the surface (photosphere) cannot be TOP "Hinode" UnveilsSolar the Mysteries of the Sun ObservingSolar Observing Satellite "Hinode" (SOLAR-B) Satelliteseen “ directly,Hinode but the upper layers ”above (SOLAR the photosphere each emit- differentB) wavelengths of lights. So, About the "Hinode" Project you can see each layer by changing the observing wavelength. By loading three telescopes observing in "Hinode" Unveils Solar Observing Satellite "Hinode" (SOLAR-B) different wavelengththe Mysteries ranges, of the Hinode can simultaneously observe from the photosphere to the corona (upper atmosphere).Sun Characteristics of the Advanced Telescopes Overview of “Hinode” -
A New Vla–Hipparcos Distance to Betelgeuse and Its Implications
The Astronomical Journal, 135:1430–1440, 2008 April doi:10.1088/0004-6256/135/4/1430 c 2008. The American Astronomical Society. All rights reserved. Printed in the U.S.A. A NEW VLA–HIPPARCOS DISTANCE TO BETELGEUSE AND ITS IMPLICATIONS Graham M. Harper1, Alexander Brown1, and Edward F. Guinan2 1 Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80309, USA; [email protected], [email protected] 2 Department of Astronomy and Astrophysics, Villanova University, PA 19085, USA; [email protected] Received 2007 November 2; accepted 2008 February 8; published 2008 March 10 ABSTRACT The distance to the M supergiant Betelgeuse is poorly known, with the Hipparcos parallax having a significant uncertainty. For detailed numerical studies of M supergiant atmospheres and winds, accurate distances are a pre- requisite to obtaining reliable estimates for many stellar parameters. New high spatial resolution, multiwavelength, NRAO3 Very Large Array (VLA) radio positions of Betelgeuse have been obtained and then combined with Hipparcos Catalogue Intermediate Astrometric Data to derive new astrometric solutions. These new solutions indicate a smaller parallax, and hence greater distance (197 ± 45 pc), than that given in the original Hipparcos Catalogue (131 ± 30 pc) and in the revised Hipparcos reduction. They also confirm smaller proper motions in both right ascension and declination, as found by previous radio observations. We examine the consequences of the revised astrometric solution on Betelgeuse’s interaction with its local environment, on its stellar properties, and its kinematics. We find that the most likely star-formation scenario for Betelgeuse is that it is a runaway star from the Ori OB1 association and was originally a member of a high-mass multiple system within Ori OB1a. -
Michael Perryman
Michael Perryman Cavendish Laboratory, Cambridge (1977−79) European Space Agency, NL (1980−2009) (Hipparcos 1981−1997; Gaia 1995−2009) [Leiden University, NL,1993−2009] Max-Planck Institute for Astronomy & Heidelberg University (2010) Visiting Professor: University of Bristol (2011−12) University College Dublin (2012−13) Lecture program 1. Space Astrometry 1/3: History, rationale, and Hipparcos 2. Space Astrometry 2/3: Hipparcos science results (Tue 5 Nov) 3. Space Astrometry 3/3: Gaia (Thu 7 Nov) 4. Exoplanets: prospects for Gaia (Thu 14 Nov) 5. Some aspects of optical photon detection (Tue 19 Nov) M83 (David Malin) Hipparcos Text Our Sun Gaia Parallax measurement principle… Problematic from Earth: Sun (1) obtaining absolute parallaxes from relative measurements Earth (2) complicated by atmosphere [+ thermal/gravitational flexure] (3) no all-sky visibility Some history: the first 2000 years • 200 BC (ancient Greeks): • size and distance of Sun and Moon; motion of the planets • 900–1200: developing Islamic culture • 1500–1700: resurgence of scientific enquiry: • Earth moves around the Sun (Copernicus), better observations (Tycho) • motion of the planets (Kepler); laws of gravity and motion (Newton) • navigation at sea; understanding the Earth’s motion through space • 1718: Edmond Halley • first to measure the movement of the stars through space • 1725: James Bradley measured stellar aberration • Earth’s motion; finite speed of light; immensity of stellar distances • 1783: Herschel inferred Sun’s motion through space • 1838–39: Bessell/Henderson/Struve -
Cmes, Solar Wind and Sun-Earth Connections: Unresolved Issues
CMEs, solar wind and Sun-Earth connections: unresolved issues Rainer Schwenn Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, Germany [email protected] In recent years, an unprecedented amount of high-quality data from various spaceprobes (Yohkoh, WIND, SOHO, ACE, TRACE, Ulysses) has been piled up that exhibit the enormous variety of CME properties and their effects on the whole heliosphere. Journals and books abound with new findings on this most exciting subject. However, major problems could still not be solved. In this Reporter Talk I will try to describe these unresolved issues in context with our present knowledge. My very personal Catalog of ignorance, Updated version (see SW8) IAGA Scientific Assembly in Toulouse, 18-29 July 2005 MPRS seminar on January 18, 2006 The definition of a CME "We define a coronal mass ejection (CME) to be an observable change in coronal structure that occurs on a time scale of a few minutes and several hours and involves the appearance (and outward motion, RS) of a new, discrete, bright, white-light feature in the coronagraph field of view." (Hundhausen et al., 1984, similar to the definition of "mass ejection events" by Munro et al., 1979). CME: coronal -------- mass ejection, not: coronal mass -------- ejection! In particular, a CME is NOT an Ejección de Masa Coronal (EMC), Ejectie de Maså Coronalå, Eiezione di Massa Coronale Éjection de Masse Coronale The community has chosen to keep the name “CME”, although the more precise term “solar mass ejection” appears to be more appropriate. An ICME is the interplanetry counterpart of a CME 1 1. -
Astrometry and Optics During the Past 2000 Years
1 Astrometry and optics during the past 2000 years Erik Høg Niels Bohr Institute, Copenhagen, Denmark 2011.05.03: Collection of reports from November 2008 ABSTRACT: The satellite missions Hipparcos and Gaia by the European Space Agency will together bring a decrease of astrometric errors by a factor 10000, four orders of magnitude, more than was achieved during the preceding 500 years. This modern development of astrometry was at first obtained by photoelectric astrometry. An experiment with this technique in 1925 led to the Hipparcos satellite mission in the years 1989-93 as described in the following reports Nos. 1 and 10. The report No. 11 is about the subsequent period of space astrometry with CCDs in a scanning satellite. This period began in 1992 with my proposal of a mission called Roemer, which led to the Gaia mission due for launch in 2013. My contributions to the history of astrometry and optics are based on 50 years of work in the field of astrometry but the reports cover spans of time within the past 2000 years, e.g., 400 years of astrometry, 650 years of optics, and the “miraculous” approval of the Hipparcos satellite mission during a few months of 1980. 2011.05.03: Collection of reports from November 2008. The following contains overview with summary and link to the reports Nos. 1-9 from 2008 and Nos. 10-13 from 2011. The reports are collected in two big file, see details on p.8. CONTENTS of Nos. 1-9 from 2008 No. Title Overview with links to all reports 2 1 Bengt Strömgren and modern astrometry: 5 Development of photoelectric astrometry including the Hipparcos mission 1A Bengt Strömgren and modern astrometry .. -
Co-Aligned IRIS, SDO and Hinode Data Cubes Release 1.0
Co-aligned IRIS, SDO and Hinode data cubes Release 1.0 Milan Gošic´ Feb 26, 2020 CONTENTS 1 Introduction 1 1.1 About this Guide.............................................1 1.2 Synopsis of the IRIS, Hinode and SDO missions............................1 1.3 Hinode and SDO data cubes co-aligned with IRIS observations....................2 2 Finding and downloading IRIS-SDO-Hinode co-aligned data cubes5 2.1 Using the IRIS Webpage (HCR).....................................5 2.2 Using SSWIDL..............................................5 3 Reading and browsing IRIS-SDO-Hinode co-aligned data cubes 11 3.1 Reading level 2 co-aligned SDO and Hinode datasets.......................... 11 3.2 Browsing co-aligned SDO and Hinode data cubes with CRISPEX................... 13 i ii CHAPTER ONE INTRODUCTION 1.1 About this Guide The purpose of this guide is to provide detailed instructions on how users can find, download, browse, and analyze co-aligned level 2 data obtained with The Interface Region Imaging Spectrograph (IRIS), the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO), and Hinode/SOT level 2 data. The IRIS team at the Lockheed Martin Solar and Astrophysics Laboratory (LMSAL) created new data cubes consisting of the Hinode/SOT and SDO/AIA images co-aligned with the simultaneous IRIS observations. These datasets all have the same IRIS level 2 FITS format, therefore can be accessed and examined using the IRIS SolarSoft software. In this guide, we provide step by step instructions how to access, read, and visualize these newly created co-aligned data cubes. In particular, we describe: • How to find data using SolarSoft IDL routines; • How to acquire data sets using either SolarSoft or Heliophysics Coverage Registry (HCR); • How to read data and visualize them using SolarSoft routines or Crisp Spectral Explorer (CRISPEX). -
Development of 60Μm Pitch Cdte Double-Sided Strip Detector for FOXSI-3 Rocket Experiment
Development of 60µm pitch CdTe double-sided strip detector for FOXSI-3 rocket experiment Kento Furukawa(U-Tokyo, ISAS/JAXA) Shin'nosuke Ishikawa, Tadayuki Takahashi, Shin Watanabe(ISAS/JAXA), Koichi Hagino(Tokyo University of Science), Shin'ichiro Takeda(OIST), P.S. Athiray, Lindsay Glesener, Sophie Musset, Juliana Vievering (U. of Minnesota), Juan Camilo Buitrago Casas , Säm Krucker (SSL/UCB), and Steven Christe (NASA/GSFC) 1 2 CdTe semiconductor and diode device Cadmium Telluride semiconductor : • High density • Large atomic number • High efficiency Issue : small µτ product especially for holes 260eV(FWHM) • Uniform & thin device @6.4keV 1400V,-40℃ • Schottky Diode (Takahashi et al. 1998 ) High bias voltage full charge collection + high energy resolution Takahashi et al. (2005) 3 Application of CdTe Diode Double-sided Strip Detector Watanabe et al. 2009 Anode(Pt): Ohmic contact Cathode(Al): Schottky contact Astrophysical Application • Hard X-ray Imager(HXI) onboard Hitomi(ASTRO-H) satellite • FOXSI rocket mission Medical Application • Small animal SPECT system (OIST/JAXA) 4 Hard X-ray study of the Sun Observation Target : the Sun Corona and flare Scientific Aim • Coronal Heating (thermal emission) • Particle Acceleration (non-thermal emission ) →Sensitive Hard X-ray imaging and spectral observation is the key especially for small scale flares study Soft X-ray image by Hinode (micro and nano) (NAOJ/JAXA) So far only Indirect Imaging e.g. RHESSI spacecraft (Rotational Modulation collimator) No direct imaging in hard X-ray band for solar mission 5 FOXSI rocket mission FOXSI experiment (UCB/SSL, NASA, UMN, ISAS/JAXA) Indirect Direct Imaging Spectroscopy with Focusing Optics in Hard X-ray Hard X-ray telescopes + CdTe focal plane detectors FOXSI’s hard X-ray telescope clearly identified a micro-flare with high S/N ratio Direct Telescope Angular resolution : 5 arcsec (FWHM) Focal plane detector 50µm on focal plane Krucker et al. -
Message from the Director General September 2017 Saku Tsuneta Director General
Message from the Director General September 2017 Saku Tsuneta Director General Institute of Space and Astronautical Science Japan Aerospace Exploration Agency On April 28, 2016, the Japan former ISAS project managers, and levels, the satellite was declared to Aerospace Exploration Agency an Action Plan for Reforming ISAS have entered into its scheduled orbit (JAXA) made the difficult decision Based on the Anomaly Experienced in March 2017. The successful start to terminate attempts to restore by Hitomi was developed. In of the ARASE mission is a testament communication with the X-ray addition, “town hall meetings” were to the dedication and skills across Astronomy Satellite ASTRO-H (also held to share the spirit and practice JAXA. known as HITOMI), which was of the action plan with all ISAS ISAS is currently operating six launched on February 17, 2016, due employees. The plan, which was satellites and space probes: ARASE, to the communication anomalies applied to launch preparations of Hayabusa2, HISAKI, AKATSUKI, that occurred on March 26, 2016. the geospace exploration satellite HINODE, and GEOTAIL. Asteroid Since that time, in consultation with ARASE, contributed to the successful Explorer Hayabusa2, which is experts inside as well as outside and stable operation of that satellite, currently on its planned trajectory JAXA, the Institute of Space and and will be applied to other projects towards the 162173 Ryugu asteroid Astronautical Science (ISAS) has such as the Smart Lander for under ion engine power, is equipped been making every possible effort Investigating Moon (SLIM). The plan- with new technologies for solar to determine what went wrong, and do-check-act (PDCA) cycle should system exploration such as long- what can be done to prevent this work to further refine both current distance communication using Ka- from happening again in the future. -
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 -
The History of Solar
Solar technology isn’t new. Its history spans from the 7th Century B.C. to today. We started out concentrating the sun’s heat with glass and mirrors to light fires. Today, we have everything from solar-powered buildings to solar- powered vehicles. Here you can learn more about the milestones in the Byron Stafford, historical development of solar technology, century by NREL / PIX10730 Byron Stafford, century, and year by year. You can also glimpse the future. NREL / PIX05370 This timeline lists the milestones in the historical development of solar technology from the 7th Century B.C. to the 1200s A.D. 7th Century B.C. Magnifying glass used to concentrate sun’s rays to make fire and to burn ants. 3rd Century B.C. Courtesy of Greeks and Romans use burning mirrors to light torches for religious purposes. New Vision Technologies, Inc./ Images ©2000 NVTech.com 2nd Century B.C. As early as 212 BC, the Greek scientist, Archimedes, used the reflective properties of bronze shields to focus sunlight and to set fire to wooden ships from the Roman Empire which were besieging Syracuse. (Although no proof of such a feat exists, the Greek navy recreated the experiment in 1973 and successfully set fire to a wooden boat at a distance of 50 meters.) 20 A.D. Chinese document use of burning mirrors to light torches for religious purposes. 1st to 4th Century A.D. The famous Roman bathhouses in the first to fourth centuries A.D. had large south facing windows to let in the sun’s warmth. -
Arxiv:0710.2934V2 [Astro-Ph] 17 Oct 2007
PASJ: Publ. Astron. Soc. Japan , 1–??, c 2018. Astronomical Society of Japan. A Tale Of Two Spicules: The Impact of Spicules on the Magnetic Chromosphere Bart De Pontieu1, Scott McIntosh2,3, Viggo H. Hansteen4,1, Mats Carlsson4 [email protected], [email protected], [email protected],[email protected] C.J. Schrijver1, T.D. Tarbell1, A.M. Title1, R.A. Shine1 [email protected], [email protected], [email protected], [email protected] Y. Suematsu5, S. Tsuneta5, Y. Katsukawa5, K. Ichimoto5, T. Shimizu6 S. Nagata7 [email protected],[email protected], [email protected], [email protected], [email protected], [email protected] 1Lockheed Martin Solar and Astrophysics Laboratory, Palo Alto, CA 94304, USA 2High Altitude Observatory, National Center for Atmospheric Research, PO Box 3000, Boulder, CO 80307, USA 3Department of Space Studies, Southwest Research Insititute, 1050 Walnut St, Suite 400, Boulder, CO 80302, USA 4Institute of Theoretical Astrophysics, University of Oslo, PB 1029 Blindern, 0315 Oslo Norway 5National Astronomical Observatory of Japan, Mitaka, Tokyo, 181-8588, Japan 6ISAS/JAXA, Sagamihara, Kanagawa, 229-8510, Japan 7Kwasan and Hida Observatories, Kyoto University,Yamashina, Kyoto, 607-8471, Japan (Received 2007 June 10; accepted accepted for Hinode special issue) Abstract We use high-resolution observations of the Sun in Ca II H (3968A)˚ from the Solar Optical Telescope on Hinode to show that there are at least two types of spicules that dominate the structure of the magnetic solar chromosphere. Both types are tied to the relentless magnetoconvective driving in the photosphere, but have very different dynamic properties.