IMPRS June 2003. The Nobeyama (Japan) radioheliograph Large antenna arrays are needed for imaging objects on the sky in radiofrequencies, also for imaging.

Slides:

Advertisements

Similar presentations

ELECTRICAL, THERMAL AND MECHANICAL PROPERTIES OF RANDOM MIXTURES MATERIALS RESEARCH CENTRE DEPARTMENT OF MECHANICAL ENGINEERING UNIVERSITY OF BATH, UK.

Advertisements

Radiative Transfer Dr. X-Pol Microwave Remote Sensing INEL 6669

Prof. Ji Chen Notes 15 Plane Waves ECE Spring 2014 z x E ocean.

On the link between the solar energetic particles and eruptive coronal phenomena On the link between the solar energetic particles and eruptive coronal.

Master Programme in Space Engineering 300 ECTS = 5 year Luleå 2,5 year + Kiruna 2 year + Master thesis project 1/2 år Courses of ECTS = 5 weeks (some 15.

Global Properties of Heliospheric Disturbances Observed by Interplanetary Scintillation M. Tokumaru, M. Kojima, K. Fujiki, and M. Yamashita (Solar-Terrestrial.

Surface Penetrating Radar Simulations for Jupiter’s Icy Moons Thorsten Markus, Laboratory for Hydrospheric Processes NASA/GSFC,

Strength of Coronal Mass Ejection- driven Shocks Near the Sun and Its Importance in Predicting Solar Energetic Particle Events Chenglong Shen 1, Yuming.

M. J. Reiner, 1 st STEREO Workshop, March, 2002, Paris.

Electron Acceleration at the Solar Flare Reconnection Outflow Shocks Gottfried Mann, Henry Aurass, and Alexander Warmuth Astrophysikalisches Institut Potsdam,

Coronal IP Shocks Nat Gopalswamy NASA/GSFC Elmau CME Workshop, 2003 February 7 Plenary talk Sun Earth.

ISP Astronomy Gary D. Westfall1Lecture 6 The Nature of Light Light and other forms of radiation carry information to us from distance astronomical.

Chapter 5 Basic properties of light and matter. What can we learn by observing light from distant objects? How do we collect light from distant objects?

Rosetta – Unlocking the Secrets of the Solar System Dr Ross Burgon, Department of Physical Sciences, The Open University.

F1B: Determine the Dominant Processes of Particle Acceleration Phase , Open the Frontier UV Spectroscopic determin- ation of pre/post-shock density,

January Nobeyama radioheliograph visit Microwave Signatures of Fast CMEs Nat Gopalswamy NASA Goddard Space Flight Center Greenbelt MD USA.

Solar Energetic Particles -acceleration and observations- (Two approaches at the highest energy) Takashi SAKO Solar-Terrestrial Environment Laboratory,

IMPRS June The principle of time-of-flight (TOF) instruments From the 3 independently measured quantities (E/q, τ, E total ) the 3 desired quantities.

SWG-17Pasadena, CA B A Direction Finding and Triangulation from STEREO & Wind M. J. Reiner.

Sounding the Ganymede’s crust with a GPR V. Ciarletti 1, A. Le Gall 1, M. Biancheri-Astrier 2, J-J. Berthelier 1, S.M. Clifford 3, D. Plettemeier 4, M.

Stuart D. BaleFIELDS iCDR – Science Requirements Solar Probe Plus FIELDS Instrument CDR Science and Instrument Overview Science Requirements Stuart D.

Pietro Zucca, Eoin Carley, Shaun Bloomfield, Peter Gallagher

Shock wave formation heights using 2D density and Alfvén maps of the corona ABSTRACT Coronal shock waves can produce decametric radio emission known Type.

Österreichische Akademie der Wissenschaften (ÖAW) / Institut für Weltraumforschung (IWF), Graz, Austria, T +43/316/ , iwf.oeaw.ac.atDownload:2013.

Radio Remote Sensing of the Corona and the Solar Wind Steven R. Spangler University of Iowa.

Solar System Missions Division Solar Orbiter Next major Solar and Heliospheric mission ESA ILWS flagship Now with the Inner Heliospheric Sentinels.

RUSSIAN SPACE MISSIONS FOR SOLAR-TERRESTRIAL SCIENCE ILWS-2011 A.A. Petrukovich, L.M. Zelenyi Space Research Institute V.D. Kuznetsov IZMIRAN.

UNCOSS Underwater coastal sea surveyor Project meeting and workshop: UNCOSS Project partners Dubrovnik 30 th November and 01 st December 2011.

OBSERVATION OF THE JANUARY 1997 CORONAL MASS EJECTION NEAR THE SUN USING RADIO SOUNDING TECHNIQUE WITH GALILEO SPACECRAFT A.I. Efimov, L.N. Samoznaev,

IHY Workshop A PERSONAL VIEW OF SOLAR DRIVERS for Solar Wind Coronal Mass Ejections Solar Energetic Particles Solar Flares.

Remote Radio Sounding Science For JIMO J. L. Green, B. W. Reinisch, P. Song, S. F. Fung, R. F. Benson, W. W. L. Taylor, J. F. Cooper, L. Garcia, D. Gallagher,

RHESSI and Radio Imaging Observations of Microflares M.R. Kundu, Dept. of Astronomy, University of Maryland, College Park, MD G. Trottet, Observatoire.

Relation between Type II Bursts and CMEs Inferred from STEREO Observations N. Gopalswamy, W. Thompson, J. Davila, M. Kaiser NASA Goddard Space Flight Center,

Stuart D. BaleFIELDS iPDR – Science Requirements Solar Probe Plus FIELDS Instrument PDR Science and Instrument Overview Science Requirements Stuart D.

P. Harden, NA5NFDIM Dayton SOLAR ACTIVITY And HF PROPAGATION Paul Harden, NA5N For FDIM Dayton 2005.

Living With a Star Radiation Belt Storm Probes and Associated Geospace Missions D. G. Sibeck Project Scientist NASA Goddard Space Flight Center.

China National Report , Uppsala, Sweden China National Space Administration.

Solar Wind and Coronal Mass Ejections

Faraday Rotation: Unique Measurements of Magnetic Fields in the Outer Corona Justin C. Kasper (UM), Ofer Cohen (SAO), Steven Spangler (Iowa), Gaetan Le.

STEREO: Beyond 3D. Why the Sun? The sun provides energy for the development of life on our planet. Our orbit looks calm and peaceful, but there is nothing.

ESTEC 7 Dec Radio Properties of the Moon: a brief review of some important bits Graham Woan University of Glasgow.

Why Solar Electron Beams Stop Producing Type III Radio Emission Hamish Reid, Eduard Kontar SUPA School of Physics and Astronomy University of Glasgow,

Plasma - What It Is, What It isn’t A Shocking Exposé with Investigations by McGourty and Rideout.

SRS Data Examples A brief overview of some types of radio emissions observed on the Solar Radio Spectrograph.

Type III radio bursts observed with LOFAR and Nançay radioheliograph Jasmina Magdalenić 1, C. Marqué 1, A. Kerdraon 2, G. Mann 3, F. Breitling 3, C. Vocks.

InterPlanetary Scintillation IPS induced Pluripotent Stem cell iPS.

SH 51A-02 Evolution of the coronal magnetic structures traced by X-ray and radio emitting electrons during the large flare of 3 November 2003 N.Vilmer,

Hard X-ray and radio observations of the 3 June 2007 flare Nicole Vilmer Meriem Alaoui Abdallaoui Solar Activity during the Onset of Solar Cycle

-1- Coronal Faraday Rotation of Occulted Radio Signals M. K. Bird Argelander-Institut für Astronomie, Universität Bonn International Colloquium on Scattering.

What Channel is That?.  Visible light is a form of electromagnetic radiation.  Others include:  Radio waves  Infrared waves (heat)  Ultraviolet waves.

Coronal scattering under strong regular refraction Alexander Afanasiev Institute of Solar-Terrestrial Physics Irkutsk, Russia.

The Space Weather Week Monique Pick LESIA, Observatoire de Paris November 2006.

SOLAR RADIO PHYSICS RESEARCH IN INDONESIA

Radio Sounding of the Near-Sun Plasma Using Polarized Pulsar Pulses I.V.Chashei, T.V.Smirnova, V.I.Shishov Pushchino Radio Astronomy Obsertvatory, Astrospace.

Mission Description Well-designed spacecraft and instruments using high energy launches and gravity assists to escape quickly Could be accomplished by.

Type IV Radio Bursts and Source Regions Observed by NoRH: Results Sara Petty, CUA/ GSFC Advisor: Dr. Nat Gopalswamy Type IV Radio Bursts Revisited Research.

RPWI Team Meeting, Sep. 2010, Roma Magnetic Loop Antenna (MLA) Scientific Objectives A. Marchaudon, V. Krasnoselskikh, T. Dudok de Wit, C. Cavoit,

FUTURE OBSERVATIONS OF THE OUTER HELIOSPHERE M. Hilchenbach and H. Rosenbauer Max-Planck-Institut für Aeronomie, D Katlenburg-Lindau, Germany.

Stuart D. BaleFIELDS SOC CDR – Science Requirements Solar Probe Plus FIELDS SOC CDR Science and Instrument Overview Science Requirements Stuart D. Bale.

Solar observations with single LOFAR stations C. Vocks 1. Introduction: Solar Radio radiation 2. Observations with single LOFAR stations 3. Spectrometer.

Presented by G. Hena Mercy Sugirthem G. Hena Mercy Sugirthem M. Sharmila M. Sharmila.

Complexity of Solar Eruptions Nat Gopalswamy, NASA GSFC, Greenbelt, MD

Cassini Huygens EECS 823 DIVYA CHALLA.

An Introduction to Observing Coronal Mass Ejections

Solar and heliosheric WG

Ian Richardson HILARY CANE Bruny Island and Tycho von Rosenvinge

SESAME: Surface Electric Sounding and Acoustic Monitoring Experiment

Solar Radio Imaging Array SIRA

Solar Probe Plus FIELDS Instrument PSR - MEP Introduction

Steven R. Spangler University of Iowa

Presentation transcript:

IMPRS June 2003

The Nobeyama (Japan) radioheliograph Large antenna arrays are needed for imaging objects on the sky in radiofrequencies, also for imaging the sun in radiofrequencies

IMPRS June 2003 Radiobursts from the Sun

IMPRS June 2003 Most spacecraft carry electric dipole antennae The Helios solar probes

IMPRS June 2003

The emitted radiofrequency reveals the local plasma density, And, knowing the radial density profile, the distance of the emitting region to the Sun

IMPRS June 2003 A classcical Type III radio burst: energetic electrons progressing out from the Sun

IMPRS June 2003

Radio signals („bursts“) as remote sensors

IMPRS June 2003

„Solar Cosmic Rays“ cause radio bursts

IMPRS June 2003 Height-time diagram of the May 3rd, 1999, CME, as determined from LASCO, and from drift rates of type II radio emission. The CME shock runs ahead of and simultaneously to the metric type II shock. They cannot be the same! Radio signals („bursts“) as remote sensors Maybe they can!

IMPRS June 2003 Where the heliosphere ends Radio signals from the heliopause!

IMPRS June 2003 Where the heliosphere ends Radio signals from the heliopause!

IMPRS June 2003 The ROSETTA Mission (with PhD student M. Benna)

IMPRS June 2003 The CONSERT Experiment Sonde Nucleus (?) VHF (90 MHz) Roland Internal permittivity of the nucleus Structure and composition of the nucleus Phase and Attenuation Data  Principal Investigator : Dr. Wlodek Kofman (LPG -France)  Countries : Germany, Italy, USA,Norway, Netherlands & UK  Masses : 2900 g  Orbiter 1900 g  lander  DC Power : 3 W  Orbiter 2 W  Lander  Frequency : 85 MHz à 95 MHz  HF Power: 2,0 W  Orbiter 0,2 W  lander  Data points / orbit : 3000

IMPRS June 2003 Computation of dielectric properties... Porosity Distribution Density distribution Maxwell-Granett Mixing Laws Sihvola & Kong* 3 components : silicates, water ice & voids Dielectric permittivity distribution (at 100 MHz) Dielectric Absorption (at 100 MHz) * Shivola A. & Kong J., 1988, IEEE Trans. Geo. & Rem. Sens., 26, p

IMPRS June 2003