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INTERBALL Auroral Results Page

Auroral Probe Results Page


Below is a table of INTERBALL-2 experiments summary to remind you about specific features of each instrument. Click on the name of an appropriate instrument to see some samples of data processing.
See bottom of the page for additional information.

Experiment Measured Parameters PI And Key Scientists
AURORAL PLASMA
S K A - 3 Spectra of electrons and ions 0.03 < E < 15 keV; anisotropy of electrons and ions (M = 1, 4, 16), 30 < E < 500 keV/Q F. Shuiskaya  
A. Kuzmin  
Yu. Galperin 
R. Kovrazhkin 
V. Stepanov 
IKI, Moscow, Russia
I O N Electron and ion spectra and anisotropy (M = 1, 2, 4, 16), 0.005 < E < 20 keV/Q J. A. Sauvaud 
CESR, Toulouse, France 
R. Kovrazhkin 
K. Afanasiev 
IKI, Moscow, Russia
PROMICS-3 Ion composition (M = 1-32) and 3-D energy distribution, 10 eV < E < 30 keV/Q I. Sandahl  
IRF, Kiruna, Sweden 
E. Budnik  
N. Pissarenko  
E. Dubinin  
IKI, Moscow, Russia 
H. Koskinen  
T. Pulkkinen  
FMI, Helsinki, Finland
THERMAL PLASMA
HYPERBOLOID Ion composition and 3-D distribution functions, M = 1-32 (with H+, He+, O++, O+ routinely), 0.1 < E < 80 eV N. Dubouloz 
J. -J. Berthelier  
CETP, Saint-Maur, France 
Yu. Galperin 
T. Muliarchik  
D. Chugunin 
IKI, Moscow, Russia
K M - 7 Temperature of cold electrons, T < 10 eV J. Smilauer  
Inst. of Atm. Physics CAS, 
Prague, Czech. Republic 
V. Afonin  
IKI, Moscow, Russia
ALPHA-3 Thermal plasma ion flux, E < 25 eV/Q V. Bezrukikh  
IKI, Moscow, Russia
WAVES AND FIELDS
I M A P - 3 Magnetic field (three components). Range 1-±70000 nT, band 0-10 Hz. I. Arshinkov  
SDS, Sofia, Bulgaria 
L. Zhuzgov  
V. Styazhkin  
IZMIRAN, Troitsk, Russia
I E S P - 2M DC electric field and ULF waves (0.1-30 Hz) S. Perraut  
CETP, Saint-Maur, France 
M. Mogilevsky 
IKI, Moscow, Russia
POLRAD Auroral kilometric radiation (20 kHz - 2 MHz) J. Hanasz 
Space Research Centre PAS, 
Torun, Poland 
M. Mogilevsky 
T. Romantsova  
IKI, Moscow, Russia
M E M O Electromagnetic waves in wide band (quantitative analysis) < 240 kHz F. Lefeuvre  
LPCE, Orleans, France 
M. Mogilevsky 
IKI, Moscow, Russia
NVK-ONCH VLF electromagnetic waves 20 Hz - 20 kHz A. Goljavin  
IZMIRAN, Troitsk, Russia 
M. Mogilevsky 
IKI, Moscow, Russia
ENERGETIC PARTICLES
D O K - 2 Energy spectra, angular distributions and time variations of electrons (E = 15-400 keV) andions (E = 20-1000 keV) K. Kudela  
Inst. of Experim. 
Physics SAS, 
Kosice, Slovakia 
V. Lutsenko  
IKI, Moscow, Russia 
E. Sarris  
University of Thrace, 
Xanthi, Greece
S/C POTENTIAL CONTROL
R O N Space electric potential control by two ion beams (N2+, In+). Ion beam currents Ibeam=0-15mkA. W. Riedler  
K. Torkar  
Space Res. Inst., Austrian 
Acad. Sci., Graz, Austria 
R. Schmidt  
ESA/ESTEC, 
Nordwijk, The Netherlands 
Yu. Galperin 
M. Veselov  
IKI, Moscow, Russia
OPTICAL OBSERVATIONS
U V A I UV auroral imager (140 - 160 nm) L. Cogger  
Univ. of Calgary, Canada 
Yu. Galperin  
M. Veselov  
IKI, Moscow, Russia
UFSIPS UV auroral oxygen emissions 130.4, 135.6, 149.3 nm in the footprint regionof the Earth's atmosphere A. Kuzmin  
IKI, Moscow, Russia 
K. Palazov  
Observ. Yuri Gagarin, 
Stara Zagora, Bulgaria
TECHNOLOGICAL EXPERIMENTS
R D - 1M Dosimetric measurements V. Bengin  
V. Petrov  
IMBP, Moscow, Russia 
S. Kuznetsov  
Moscow University, 
Moscow, Russia
A N O D Comparison of different models of solar panels A. Kozlov  
State Scientific-industrial 
corporation QUANT, 
Moscow, Russia 
T. Muliarchik  
IKI, Moscow, Russia
SERVICE SYSTEMS
BNK, BNTR, 
BNTS
Communication blocks J. Dikareva  
IKI, Moscow, Russia
S S N I Telemetry system L. Chesalin  
IKI, Moscow, Russia
S T O Telemetry system L. Bodnar  
Politechn. Inst. 
Budapest, Hungary 
J. Vojta  
Inst. of Atm. Phys. CAS, 
Prague, Czech. Republik 
S. Roishik  
Aviation Inst., Warsaw, Poland 
G. Terekhin  
IKI, Moscow, Russia
B N S Attitude processor J. Klas  
Inst. of Atm. Phys. CAS, 
Prague, Czech. Republik 
N. Eismont  
Yu. Lisakov  
IKI, Moscow, Russia

This page is designed at Space Plasma Physics Department, IKI . Please send your comments and suggestions about this page and subsequent pages to Vladimir Stepanov (see SKA-3 experiment also), or contact appropriate instrument group directly.

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