N. André, I. Mueller-Wodarg, P. Garnier, P. Louarn

RPWI Kick-Off Meeting, Uppsala, Sweden, November 26-27 2009

JupiterAvailable Datasets

EJSM: MAGNETOSPHERIC AND PLASMA SCIENCE

JEO Instruments

Radio Science

Laser Altimeter

Ice Penetrating Radar

VIS-IR Spectrometer

Camera Package

Narrow Angle Camera

Thermal Instrument

UV Spectrometer

Ion & Neutral Mass Spectrometer (sputtering)

Magnetometer

Particle and Plasma Instrument

73 kg core payload:JGO Instruments

Ka-band Transponder + Ultra Stable Oscillator

Laser Altimeter

Sub-surface Radar Sounder (radio noise, TEC?)

Wide Angle and Medium Resolution Camera

Narrow Angle Camera

VIS/IR Hyperspectral Imaging Spectrometer

Sub-millimeter wave sounder

UV Imaging Spectrometer (aurorae, Io torus)

Magnetometer

Plasma Package + Ion & Neutral Mass Spectrometer

Radio and Plasma Wave Instrument

Plan

etary

Fields

Imag

ing

MAP

S

AVAILABLE DATA AT JUPITER

Source: NASA/PDS, APL, …

Limited to archiving alone, not always L2 parametersA few radio occultation data at PDS, but limited to Jupiter and Io (contact Kliore)

Source: NASA/ESA

Pioneer 10/11 MAG PA CPI/CRT/GTT D&G+ONERAVoyager 1/2 MAG PLS LECP/CRS PWS D&G+ONERAUlysses MAG SWOOPS EPAC URAP Io torus (QTN)

(Moncuquet, PhD)Galileo MAG PLS EPD/HIC PWS Magnetic Field GIRE (JPL)

Radio Science

Cassini/Huygens MAG CAPS MIMI RPWS Radio SpectrumNew Horizons SWAP PEPSSI

1. Data 2. Models 3. Radiation

http://pds-ppi.igpp.ucla.edu/

AVAILABLE RADIO DATA AT JUPITER: SPACE-SEGMENT

Cecconi, B., N. André, andthe EJSM-EM Sensor study TeamEJSM Workshop #2, APL, 07/2009

AVAILABLE RADIO DATA AT JUPITER: DECAMETRIC (inputs from H. Rucker, 2008)

Ukrainian T-shaped Radio telescope UTR-2, Kharkov, Ukraine http://www.ri.kharkov.ua/index.html

The Ukrainian T-shaped Radio telescope, second modification (UTR-2) is the world's largest radio telescope at decameter wavelengths. The UTR-2 comprises 2040 array elements in two arms: north-south (1800×60 m) and west-east (900×60 m). It has a collective area of 150,000 square meters, and a resolution of about 40'×40' at the middle frequency 16.7 MHz. The operating frequency range is 10-28 MHz. The sensitivity is about 10 Jansky. The telescope is a part of the Ukrainian decametric VLBI system URAN, which includes another four radio telescopes of smaller size. The system has bases from 40 to 900 km.

Corresponding data archive: Space Research Institute, Graz, AustriaInvolved personnel: Alexander KONOVALENKO akonov@ri.kharkov.ua Observatoire de Nancay, Réseau Décamétrique Nançay http://www.obs-nancay.fr/

The decametric array of Nancay (Reseau Decametrique Nancay, RDN) is dedicated to the study of the electromagnetic radio emission of Jupiter, the sun and the stars. The instrument operates between 10-80 MHz, and consists of 144 helical antennas, distributed over an area of 10,000 square meter. The 8 conducting wires on each antenna have been wound in a spiral pattern on a conical surface. They are wound in either a left- or a right-handed winding spiral pattern, making them sensitive to either left- or right-hand circularly polarized radio waves. Available data: Jupiter-Quicklooks, gif-files, RHP/LHP, 10-40 MHz, from 1990-2008: http://www.obs-nancay.fr/a_index.htmProbability of occurrence of Io control emissions of Jupiter for site of Nancay, 1990-2008: http://www.obs-nancay.fr/a_index.htmInvolved personnel: Philippe ZARKA philippe.zarka@obspm.fr, Alain LECACHEUX alain.lecacheux@obspm.fr

AVAILABLE RADIO DATA AT JUPITER: DECAMETRIC (list not exhaustive)

University of Florida Radio Observatory http://ufro1.astro.ufl.edu/

Log-spiral Array: The main antennas used at UFRO for monitoring the Jovian Decametric Emission are two arrays of conical log spiral elements. Each array has eight elements; one array is right-hand and the other left-hand circularly polarized. Each conical log spiral element (TP) is about 8 meters tall and has a diameter of about 5 meters at the base. The TP is a broad band element and has been designed to work over a wide range of frequencies. For monitoring the Jovian Decametric Emission the UFRO TP arrays are used in the frequency range from 18 to 40 MHz. The arrays have a fixed beam array in the E-W direction but it can be phase-steered in the N-S direction. The E-W half-power beam width is about 90 degrees and allows the observation of Jupiter for a total of about 6 hours (+/- 3 hours around transit). Available data: http://ufro1.astro.ufl.edu/ufro/Involved personnel: C.A. HIGGINS < higgins@nssdc.gsfc.nasa.gov>, F. REYES <reyes@astro.ufl.edu> LOFAR (Low Frequency ARray) http://www.lofar.org/

LOFAR is a (future) radio telescope network, using an array of simple omni-directional antennas centered at Exloo, NL, with planned outpost radio stations in Germany (part of them already deployed), France, UK, Poland, Italy, and other EU countries. LOFAR consists of a large number of distributed low-cost wire antennas and will make observations in the frequency ranges 30–80 MHz, and 120–240 MHz, with the intended French LOFAR superstation (LSS) the frequency is extended down to 10 MHz.

Further personnel involved in (low-frequency) radio astronomy: H.O. RUCKER rucker@oeaw.ac.at, M.Y. BOUDJADA mohammed.boudjada@oeaw.ac.at, K. IMAI imai@ee.kochi-ct.ac.jp, P. ZARKA

 

AVAILABLE RADIO DATA AT JUPITER: SYNCHROTRON DATA

Santos-Costa and Bolton, JGR, 2008

VLA observations made at various wavelengths (e.g., 20 and 6 cm) http://archive.cv.nrao.edu/

Next year:• Proposal for a Jupiter Plasma Science Archive at CDPP

AMDA (Automated Multi-Dataset Analysis)

1. Visualization editor

3. Parameter editor

2. Download data

5.Visual search

4. External data

6. Conditional search

7. Time-Table manager

EJSM: RADIO (Zarka & Cecconi, JGR, 2004)73 kg core payload:

CassiniRPWSData

EJSM: MAGNETOSPHERE73 kg core payload:

4x103 (Io torus) <10-3 (outer magnetosphere) cm-3

Richards et al., AGU, 2003 Galileo PWS observations Barnhart et al., JGR, 2009

Average densities at the center of the current sheet:

@20 Rj: 1 cm-3

@120 Rj: 0.01 cm-3

Jupiter Ganymede Orbiter:

10-3 (10-4)-10 (102) cm-3

EJSM: CALLISTO73 kg core payload:

Galileo Callisto Flybys, Kliore et al., JGR, 2002Radio occultation data (2.5 GHz, S-band)

Ionospheric densities :Density above 104 cm-3 for very close flybys (< 50 km)

Galileo Ganymede FlybysEviatar et al., PSS, 2001Gurnett et al., Nature, 1996

Ionospheric densities :

Observed density: ~2x102 cm-3 @ ~260 kmInferred density: 4x102 cm-3 @ surfaceUpper limit: 4x103 cm-3 @ surface

(radio occultations, Kliore et al., 1998)Ion temperature: 1-3 eV (Frank et al., GRL, 1997)

EJSM: GANYMEDEA radio source 73 kg core payload:

GalileoPWS data

EJSM: GANYMEDE

EJSM: GANYMEDE GalileoPWSData

Das2 software from Iowa