Interrelation between Cosmic Rays, Magnetosphere Interrelation between Cosmic Rays, Magnetosphere particles and the Earth Atmospheric Phenomena-particles and the Earth Atmospheric Phenomena-Prospects of Experimental Study from SatellitesProspects of Experimental Study from Satellites

M.I. PanasyukM.I. Panasyuk

D.V. Skobeltsyn Institute of Nuclear Physics of D.V. Skobeltsyn Institute of Nuclear Physics of

M.V. Lomonosov Moscow State UniversityM.V. Lomonosov Moscow State University

Content.

1. Historical remarks. Scientific goals.2. Plans for complex studies on satellites: - RELEC mission - Tatiana-2 mission. - TUS mission3. Conlusion

Discovery of electron radiation belts onboard Discovery of electron radiation belts onboard ELECTRON satellites in 60’s.ELECTRON satellites in 60’s.

MAXIS (1996) experiment onboard balloons, MAXIS (1996) experiment onboard balloons, Kiruna. High-energy electronsKiruna. High-energy electrons >500>500 keV keV precipitations: precipitations:

Flux -Flux - 55 х 10 х 102525 particles for eight days was particles for eight days was detected at low altitudes .detected at low altitudes .

Total number of trapped electrons – 2Total number of trapped electrons – 2 х 10 х 102525..

History of the problemHistory of the problem

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

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

Scientific goalsScientific goals

Magnetosphere relativistic electron Magnetosphere relativistic electron acceleration and precipitation research. acceleration and precipitation research. Study of high-energy particles acting in the Study of high-energy particles acting in the upper atmosphere and ionosphere.upper atmosphere and ionosphere.Search of transient phenomena in possible of transient phenomena in possible connection with energetic particle interactions connection with energetic particle interactions in the atmospherein the atmosphereStudy of acceleration processes in the atmosphere as the possible source of high energy magnetosphere electrons

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

Demands to instrumentationDemands to instrumentation

electron detectors: wide energy range (~0.1-10.0 MeV), electron detectors: wide energy range (~0.1-10.0 MeV), temporal resolution ~1 ms, pitch-angle distribution temporal resolution ~1 ms, pitch-angle distribution measuring, wide dynamical range (from ~0.1 up to measuring, wide dynamical range (from ~0.1 up to 101055 part./cm part./cm22s).s).

detecting of protons with energies > 1 MeV, detecting of protons with energies > 1 MeV, low-frequency analyzer: measuring at least of two field low-frequency analyzer: measuring at least of two field

components , frequency bands ~0.1-10 kHz.components , frequency bands ~0.1-10 kHz. X- and gamma-ray detectors: temporal resolution X- and gamma-ray detectors: temporal resolution

~1 ~1 μμs, sensitivity ~10s, sensitivity ~10-8-8 erg/cm erg/cm22 for burst. for burst. Imaging of the atmosphere in optics, UV, X- and Imaging of the atmosphere in optics, UV, X- and

gamma-rays with resolution of gamma-rays with resolution of ~km in wide FOV~km in wide FOV..

RELEC RELEC ((RRelativisticelativistic ELECELECtronstrons) ) mission.mission.

DRG-1 & DRG-2 - two identical detectors of X-, gamma-DRG-1 & DRG-2 - two identical detectors of X-, gamma-rays and high-energy electrons of high temporal rays and high-energy electrons of high temporal resolution and sensitivityresolution and sensitivity

DRG-3 - three axeDRG-3 - three axe directed detectors of energetic directed detectors of energetic electrons and protonselectrons and protons

MTEL - optical imagerMTEL - optical imager DUV - UV detectorDUV - UV detector BChK - module of charge and neutral particle detectorsBChK - module of charge and neutral particle detectors NChA - low-frequency analyserNChA - low-frequency analyser RChA - radio-frequency analyserRChA - radio-frequency analyser DOSTEL - dosimeter moduleDOSTEL - dosimeter module BSKU - module of commands and data collection BSKU - module of commands and data collection

DRG-1 (DRG-2) instrumentDRG-1 (DRG-2) instrument..

Two identical NaI(Tl)/CsI(Tl)/plastic scintillator phosvich Two identical NaI(Tl)/CsI(Tl)/plastic scintillator phosvich detectors, both directed toward the Earthdetectors, both directed toward the Earth..Physical parameters:Physical parameters:

X- and gamma-quantaX- and gamma-quanta electronselectronsenergy range energy range 0.01-2.0 MeV,0.01-2.0 MeV, 0.2-10.0 MeV0.2-10.0 MeVeffective area effective area ~200 cm~200 cm22 srsr ~200 cm ~200 cm22sr sr (total ~800 cm(total ~800 cm22))temporal resolution temporal resolution 0.1 0.1 μμss 1.0 ms1.0 mssensitivity sensitivity ~5·10~5·10-9-9 erg/cm erg/cm22 ~10 ~10-1-1 part./cm part./cm22ss

Photo-multiplier

CsI(Tl)

NaI(Tl)

Al foil

Plastic

Detector unitDetector unit

DRG-3 instrumentDRG-3 instrument

Three identical NaI(Tl)/CsI(Tl)/plastic scintillator Three identical NaI(Tl)/CsI(Tl)/plastic scintillator phosvich detectors, directed along three axe mutually phosvich detectors, directed along three axe mutually normal (as Cartesian coordinate system)normal (as Cartesian coordinate system)

Physical parameters:Physical parameters:

electronselectrons protonsprotons

energy range energy range 0.1-10.0 MeV,0.1-10.0 MeV, 1.0-100.0 MeV1.0-100.0 MeV

geom. factorgeom. factor ~2 cm~2 cm22sr sr ~2 cm~2 cm22sr sr

temporal resolution temporal resolution 1.0 ms1.0 ms 1.0 ms1.0 ms

sensitivity sensitivity ~10 part./cm~10 part./cm22ss ~10 part./cm~10 part./cm22ss

Technical parametersMass - < 4 kg;sizes 250250250 mm;power expenditure at 28 V no more 6 W.

To the skyTo the sky

Scintillation detectors

Along the geomagneticAlong the geomagneticfield linefield line

MTELMTEL instrument instrumentOptical imager based on MEMS mirror technologyOptical imager based on MEMS mirror technologyPhysical parameters (see also the talk by I.H. Park, this Physical parameters (see also the talk by I.H. Park, this workshop):workshop):

Technical parametersMass - < 5 kg;sizes 200200400 mm;power expenditure at 28V no more 6 W.

Spectral band: 300-400 nmAngle resolution: 0.4o. Angle of view: 7.5o. Cells number: 4000. Photomultiplier channels number: 64. Time resolution: 100 s. Amplitude range: 105.

BChKBChK instrument instrumentNumber of detectors for different kind of space radiation:Number of detectors for different kind of space radiation:silicon, silicon, CsICsI((TlTl), BGO, LBO, Geiger counters), BGO, LBO, Geiger counters

Physical parameters:Physical parameters:

Technical parametersMass - < 3 kg;sizes 100150150 mm;power expenditure at 28 Vno more 3 W.

Energy range:

Ee: >300 keV;

EP: >50 MeV;

Gamma: 0.05 – 1 MeV;

Neutron: 0.1 – 30 MeV

Ee: 0.1 – 5.0 MeV;

EP: 0.1 – 60 MeV;

BGO CsILBO

Charged and neutral particles Charged and neutral particles detectordetector

NChA instrumentNChA instrumentLow-frequency analyzer: two magnetic field componentLow-frequency analyzer: two magnetic field componentmeters, two electric field component meters andmeters, two electric field component meters andanalyzer unitanalyzer unit

Physical parameters:Physical parameters:

Technical parametersMass - < 3 kg;sizes 16013080 mm;power expenditure at 28 Vno more 5 W.

Frequency band: 20 Hz - 20 kHznumber of spectral components:1024frequency step: 20 Hz .Time resolution: 2 s.Number of spectral componentcategories: 16.

Magnetic and electric field component meters

ElectronsElectrons 0.2 – 10 0.2 – 10 MeVMeV

> 10 > 10 MeVMeV

>> 0.3 MeV 0.3 MeV

ProtonsProtons 0.3 – 60 MeV0.3 – 60 MeV

> 50 > 50 MeVMeV

3 – 150 MeV3 – 150 MeV

>150 >150 MeVMeV

GammaGamma 0.05 – 1.0 MeV0.05 – 1.0 MeV

NeutronNeutron 0.1 – 30 MeV0.1 – 30 MeV

X-raysX-rays 10 – 100 keV10 – 100 keV

UVUV 300-400 300-400 nmnm

Ranges of particles and quanta

TOTAL RELEC characteristicsTOTAL RELEC characteristics

MassMass 35 35 kg.kg.

PowerPower 55 55 W.W.

Data flowData flow 500 500 MBMB//day.day.

Tatiana-2 mission.Detector complex:1. Temporal profile UV+Reddetector.2. Temporal profile electron flux detector of 400 cm2 area.3. MTEL short focus UV imager, covering area in the atmosphere 160×160 km with resolution 20 km.4. MTEL long focus tracking UV imager, covering area in the atmosphere 56×56 km with resolution 7 km. 5. Temporal profile spectrometer.

1. UV-Red detector. Two PMTs covered by UV (300-400 nm) and red (600-800 nm) filters. Digital temporal signal profiles are available in time samples from 0.01 ms and up to 1 ms with duration of 128 time samples. Both PMTs has field of view (FOV)- 32º. Electronics selects TLE with the threshold of UV photons number in the atmosphere- 1021 (UV energy-0.5 KJ).

Charge particle flux detector.Area- 400 cm2 . Digital temporal signal profiles in numberof relativistic particles (r.p.) starting form several r.p. are available in time samples from 0.1 ms and up to 1 ms with duration of 128 time samples.

Scintillation plate

Light guide- convertorPMT

For MTEL telescope see the talk by I.H. Park in this workshop.

Tatiana-2 mission.Scientific goals.1. In nadir directon to observe different classes of TLE. How

different kind of TLE are distributed in the world map? TLE correlation with continents or ocean.

2. In which kind of TLE electrons are accelerated to high energies so that they penetrate from the atmosphere to the Tatiana-2 orbit?

3. Are there millisecond electron flux flashes at the orbit? Are they occured at conjunctive points with TLE (statistical analysis)?

4. Verification of lunar effect on the rate and brightness of TLE. Which kind of TLE are really affected by the Moon?

(See also the paper “UV data from Tatiana-1 and plans for Tatiana-2” in this workshop)

TUS Mission (2010-2012)

Main goal is detection of Extreme Energy Cosmic Rays. For this goala large mirror-concentrator is needed. Pixels cover 4000 km2 of the atmosphere (orbit height 450 km). For detection of TLE a pinhole camera is incorporated.

Satellite scientific payload:mass 60 kg, electric power 60 Wt, orientation to nadir ±3ºmirror-concentrator area 2 m2

In thunderstorm regions ionization of the atmosphere by EAS secondary particles, generated by EECR, may initiate TLE . Initial EAS will be detected by the main TUS detector and TLE will be detected by the pinhole camera. UV photon number in TLE is of the order 1022 but the EAS UV photon number is ~ 1015 .EAS signal duration is ~10-100 μs and TLE duration is ~1-10 ms.

EAS signal:

TLE signal.

The main TUS detector will be saturated. Below: the TLE is

“detected” by the 64- pixel pinhole camera.

0.3 ms 1 ms 2 ms 4 ms

The pinhole camera event expected to follow in time the EAS event in the main TUS detector.

Conclusion.

Complex satellite observations of particle flux at the orbit (heights of 400-1000 km) and of different kind of radiation from the atmosphere will give key evidence for the interrelation between atmospheric phenomena, magnetosphere particle flux and cosmic rays.