RELEC project (Relativistic ELECtrons)

Unified platform “Karat” for small spacecraft 2 MICROSATELLITE KARAT FOR PLANETARY MISSIONS, ASTROPHYSICAL AND GEOPHYSICAL RESEARCH

Unified platform “Karat” for small spacecraft 3 UNIFICATED SPACECRFAFT KARAT WITH PAYLOAD Spacecraft mass on the orbit – 110 kg Three-axes orientation Active operational time of a mission no lesss than 3 years

Unified platform “Karat” for small spacecraft 4 VIBRO-DYNAMIC TESTS

Unified platform “Karat” for small spacecraft 5

6 TEST ‘S FACILITY

Unified platform “Karat” for small spacecraft 7 already tested and elaborated Russian on-board systems, instruments, modules and units are used; design and interfaces are made in accordance wuth international standards; module construction of small spacecraft; on-board systems formed the spacecraft are also unificated. Spacecraft mass is about 100 kg Stabilisation accuracy - 4 ×10 -3 degree/s Orientation accuracy - 10·solid min Time of active operations 3 year On-board memory volume - no less than 8 GByte Scientific data transfer with the use of S-LINEwill done of ciast th wjПередача научной информации по радиолинии S- или X–диапазона Spacecraft ative is actyve 3aода BASIC PRINCIPLES OF UNIVERSAL SPACECRAFT KARAT ELABORATION

Unified platform “Karat” for small spacecraft 8 Goal of experiments: study of cosmic ray and magnetosphere energetic particle acting on the upper Atmosphere study of atmosphere transient luminous effects. EXPERIMENT RELEC ON-NOARD KARAT MISSION

Unified platform “Karat” for small spacecraft 9 Mission control and data receiving will be provide be the Mission Control Centre of Lavochkin space corporation as well as the compact ground receivers. Ground receivers with antenna diameter 3,7 and 5 m

Unified platform “Karat” for small spacecraft 10 Group launching By-pass mission DneprSoyuz RokotStart-M Special mission

 Discovery of electron radiation belts onboard ELECTRON satellites in 60’s.  MAXIS (1996) experiment onboard balloons, Kiruna. High-energy electrons >500 keV precipitations: Flux - 5 х particles for eight days was detected at low altitudes. Total number of trapped electrons – 2 х History of the problem

The X-rays (produced from ~1.7 MeV electrons) measurements showed that there are two main types of precipitation – long-term (~100 s) and short enhancements (~10 s) modulating the count rate. MAXIS measurements.

Precipitation of ~100 keV electrons from radiation belts measured in SAMPEX experiment.

Scientific objectives  Magnetosphere relativistic electron acceleration and precipitation research.  Study of high-energy particle acting on the upper Atmosphere and ionosphere.  of transient phenomena in possible connection with energetic particle interactions in the Atmosphere  Search of transient phenomena in possible connection with energetic particle interactions in the Atmosphere   Study of acceleration processes in the Atmosphere as the possible source of high energy magnetosphere electrons

Crucial demands  Simultaneous observations of energetic electron & proton flux and low-frequency electromagnetic wave intensity variations with high temporal resolution.  Fine time structure measurements of transient lightning events in optics, UV, X- and gamma rays. .  Monitor detection of charge and neutral background particles in different areas of near-Earth space.

Demands to the instruments  electron detectors: wide energy range (~ MeV), temporal resolution ~1 ms, pitch-angle distribution measuring, wide dynamical range (from ~0.1 up to 10 5 part./cm 2 s).  Low-frequency analyzer: measuring of two field components at least, frequency bands ~ kHz.  X- and gamma-ray detectors: temporal resolution ~1 mcs, sensitivity ~10 -8 erg/cm 2 for burst.  Additional: detecting of protons with energies > 1 MeV, wide-field observe of Atmosphere in optics, UV, X- and gamma-rays with possibility of imagination in optics.

Instruments  DRG-1 & DRG-2 - two identical detectors of X-, gamma- rays and high-energy electrons of high temporal resolution and sensitivity  DRG-3 - three axe directed detectors of energetic electrons and protons  Telescope-T - optical imager  DUF - UV detector  NChA - low-frequency analyser  RChA - radio-frequency analyser  DOSTEL - dosimeter module  BE - module of commands and data collection

DRG-1 (DRG-2) instrument Two identical NaI(Tl)/CsI(Tl)/plastic scintillator phosvich detectors, both directed toward the Earth Physical parameters: X- and gamma-quantaelectrons energy range MeV, MeV effective area ~200 cm 2 ~200 cm 2 sr (geom. factor) (total ~800 cm 2 ) temporal resolution 0.1 mcs1.0 ms sensitivity ~5·10 -9 erg/cm 2 ~10 -1 part./cm 2 s

Photo- multiplier CsI(Tl) NaI(Tl) Al foil Plastic Detector unit

DRG-3 instrument Three identical NaI(Tl)/CsI(Tl)/plastic scintillator phosvich detectors, directed along three axe mutually normal (as Cartesian coordinate system) Physical parameters: electronsprotons energy range MeV, MeV geom. factor ~2 cm 2 sr ~2 cm 2 sr temporal resolution 1.0 ms1.0 ms sensitivity ~10 part./cm 2 s~10 part./cm 2 s

To the sky Scintillation detectors Along the geomagnetic field line

Telesope -T instrument Optical imager based on multi-grain mirror Physical parameters: Spectral band: nm Angle resolution: 0.4 o. Angle of view:  7.5 o. Cells number: Photomultiplier channels number: 64. Time resolution: 100  s. Amplitude range: 10 5.

PMT1 PMT2

magnetic and electric field component meters

Electrons0.2 – 10 MeV > 10 MeV > 0.3 MeV Protons0.3 – 60 MeV > 50 MeV 3 – 150 MeV >150 MeV Gamma0.05 – 1.0 MeV Neutron0.1 – 30 MeV X-rays10 – 100 keV UV nm Ranges of particles and quanta measuring in RELEC experiment

TOTAL RELEC characteristics Mass45 kg. Power60 W. Data flow500 MB/day.

Other geophysical and space- physics problems can be solved using the same devices  Lithosphere-ionosphere connections (earthquakes)  Atmosphere-ionosphere connections (thunderstorms) Technical applications  Dosimetry and SEU (single event upsets) problem taking into account neutron component of radiation.