Russian-Italian Mission(RIM)

1993 - …

A.M. Galper

Rome 11.05.09

Bari Florence Frascati

Italy:TriesteNaple

sRome CNR, Florence

St. Petersburg

Russia:

Germany:Siegen

Sweden:KTH, Stockholm

RIM-PAMELARIM-PAMELA

Moscow

Moscow

Italy:

THE COSMIC RAY NUCLEI AND THE CENTRAL NERVOUS SYSTEM EXPERIMENTS ONBOARD OF THE SPACE STATIONS MIR AND ISS

(RIM—0)

Practical aspects of the LF-phenomenon

The cosmonauts must be ready to LF phenomenon during space flight, especially if it is the long space flight out of the earth magnetosphere.

LF phenomenon's, which systematically will be arising especially before slipping cosmonauts, can to bring up to tiredness condition and to decreasing of the operational capability.

LF phenomenon capable to exert on operational capability.

The low sensitivity to LF phenomenon is a good property for future crewmembers of the Mars missions.

Detector part of the SilEye apparatus

0.001

0.01

0.1

1

0.1 1 10 100

LET (keV/k)

Prob

abili

ty L

F

before LF

after LF

The fraction of particles that occurred in the LF-

window (1.2–0.2 sec. before a registered LF signal) and “anti-LF” window (defined, being 0.2–1.2 s after the LF)

as a functions of LET

Sergey Avdeev on Mir with the SilEye-2 detector mounted on the side of his head and the mask with LED’s in front of

his eyes.

SilEye-2

The ALTEINO experiment. On the left is shown the

electroencephalograph Halley, on the right the cosmic ray detector

AST.

The scheme of the electroencephalograph electrodes connections

Experiment “SilEye-3/Alteino” (April – May 2002, ISS)

A schematic view of the cosmonaut with the ALTEA system

1. Detector system consists of an helmet shaped mechanical structure holding 12 active silicon telescopes, assembled in 6 independent units;

2. Electrodes of the EEG system with 24 monopolar channels plus 4 bipolar channels.

3. Visual Stimulator

References

1. Bidoli, V., et al., Nuclear Instruments and Methods A, 1999, 424, 414.2. S.Avdeev, et all Acta Astronautica May 2002, vol 50/8 pp 511-525.3. Casolino, M., et al., Nature 422 (2003) 680.

Experiment NINA(RIM--1)

Experiments NINA 1,2

Scientific interest: Study of the nuclear and isotopic component of cosmic rays:

H - Fe --> 10--200 MeV/n (full containment)

Choice of the orbit: POLAR

so to be able to encounter differentfamilies of cosmic rays: galactic, albedo, trapped

• Launch: 10 July 1998

• Space - Base Baikonur

• End of mission: • 13th April

1999.

Satellite RESURS-01 n.4:PERIOD ~ 100 min.ALTITUDE ~ 840 km INCLINATION 98.7 deg.

MASS 2500 kg

The detectora silicon wafer 6x6 cm2 , 380 m thick with 16 strips, 3.6 mm wide in X -Y views. 32 wafers arranged in 16 planes, 1.4 cm apart. In total almost 12 mm of silicon.Lateral and Bottom AC for Full Containment mass resolution <0.15 amu for He, <0.1 amu for H energy resolution < 1 MeV

NINA mission

NINA-2 missionSatellite MITA:PERIOD ~ 100 min.ALTITUDE ~ 400 km INCLINATION 87.3 deg.MASS 170 kg

• Launch: 14 July 2000• Space - Base Plesetsk• End of mission: 15th August 2001.

ZENIT rocket Baikonur, Kazakhstan July 10 1998

COSMOS rocket

Plesetsk, Russia July 15 2000

NINA2-MITA

Sun-Earthpointing,89°, 440 km, 90’

Last scientific data in August 10, 2001, at 240 km altitude

NINA-RESURS

Earthpointing, 97°, 810 km, 100’

Solar Energetic Particles

• 9 SEP events have been detected by NINA in October 1998 -- April 1999, and analyzed;

• 14 SEP events have been detected by NINA-2 in October 2000 – August 2001

• 3He/4He ratios and energy spectra determined;

• 7 Nov. 1998 event 3He-enriched[3He/4He=(0.33± 0.006)]

• All SEPs present a 3He/4He higher than coronal values;

• Possible presence of deuterium on 24 Nov. 1998 and 19 July 2001

• nuclear interactions, which could contribute to the 3He content in SEPs

7 Nov. 1998 event3He/4He= 0.33 ± 0.006

[10--50 MeV/n]

3He-enriched

The 3He and 4He spectral indexes are:

The 3He/4He ratio increases with energy. Its low-energy extrapolation (~ 10-4) is consistent with ULEIS (ACE) [Mason, Mazur & Dwyer, ApJ, 525, L133, 1999] in the interval 0.2--2 MeV/n, which reported a value < 6x10-4.

3He --> = 2.5 ± 0.64He --> = 3.7 ± 0.3

Galactic Cosmic RaysCosmic ray abundances, with the odd-even effect, the peaks at C and O, and the relative depression of the light elements Li, Be and B

Very good agreement among SIS, CRIS and NINA results

Trapped particles mass reconstruction

The mass reconstruction confirms the presence of ‘real’ H and He isotopes in Radiation Belts. 3He is more abundant than 4He

Albedo particlesEnergy spectrum of protons of albedo origin was measured at different geomagnetic locationBehaviour of the proton flux as a function of altitude and longitude out of the South Atlantic Anomaly was studiedNINA and NINA-2 measurements revealed that 2H, 3H, 3He and 4He are a significant portion of the secondary flux above the atmosphere

L-shell<3, B>0.26 G

References

V.Bidoli, M. Casolino, M.De Pascale et al Isotope composition of secondary hydrogen and helium above the atmosphere Journal of Geophysical Research , 108, A5, 1211, 2003 •V.Bidoli, M. Casolino, M.De Pascale et al Energy spectrum of secondary protons above the atmosphere measured by the instruments NINA and NINA-2 Annales Geophysicae, 20, issue 10 (2002), 1693 (PDF) •A.Bakaldin, A.Galper, S Koldashov et al Geomagnetically trapped light isotopes observed with the detector NINA Journal of Geophysical Research, 107, N. A8 (2002), 1-8 •A. Bakaldin, A. Galper, S. Koldashov et al Light Isotope Abundances in Solar Energetic Particles measured by the Space Instrument NINA The Astrophysical Journal, 577:513–523, 2002 astro-ph/0106390 ,

Space experiment onboard small size satellite of Lavochkin Association

The project “MONICA”:

“Monitor of cosmic ray nuclei and ions”

Russian participants:Moscow Engineering Physics Institute (State University) – Leading instituteLebedev Physical Institute of RASIoffe Physical-Technical Institute of RASJoint Institute for Nuclear Research

Scientific objectives of MONICA experiment

Measurement of ionic charge states, as well as elemental, isotope composition and energy spectra of SEP fluxes from He to Ni in 10-300 MeV/n energy range for individual SEP events (including small impulsive SEP events). Measurement of ACR ion ionic charge and isotope composition, including new elements and isotopes, which have been observed on ACE (sulfur, isotopes of oxygen and neon and others); measurement of ACR energy spectra.Measurement of GCR and ACR fluxes modulation with the purpose of study of conditions of particle propagation in heliosphere.

Study of CR penetration into Earth magnetosphere under conditions of its strong disturbances during the solar-magnetosphere events.

The technique of CR ion charge measurement: The usage of Earth magnetic field as a separator of ion charge state

MONICA physical scheme

D1–D14 - silicon strip detectors

Detector Thicknesses:

D1, D2 – 100 µm

D3-D5 – 300 µm

D6-D14 – 1000 µm

SAC, AC – scintillation anticoincidence detectors

Physical and technical characteristics of MONICA spectrometer

Geometry factor 100 cm2sr

Aperture 45

Angle resolution 1

Energy range

H

CNO

Fe

7-70 MeV

15-150 MeV/n

25-290 MeV/n

Energy resolution 1%

Mass resolution

H

CNO

Fe

0.02

0.08

0.2

Resolution time 50 ns

Dead time <1 ms

Outline dimensions 650650300 mm(preliminary)

Mass 40 kg

Power consumption Not more

then 80 W

Power supply voltage 27 V

Matter in aperture Not more

then 0.05 g/cm2

Mass memory 1 Gbyte

Information downloads

not less than one per day

Small Size Satellite

Star Sensors

Place for scientific instrumentation

Experiment PAMELA (RIM--2)

MAGNETIC SPECTROMETER PAMELA1, 3, 7- TIME OF FLIGHT SYSTEM;2, 4- ANTICOINCIDENCE SYSTEM;5- SILICON STRIP TRACKER (SIX DOUBLE PLATES);6- MAGNET (FIVE SECTIONS); 8- SILICON STRIP IMAGING CALORIMETER;9- ANTICOINCIDENCE SCINTILLATOR; 10- NEUTRON DETECTOR; 11- HERMOCONTAINER.

PAMELA Spectrometer

Shower tail catcherShower tail catcherScintillatorScintillator

ToFToF

Magnetic Magnetic spectrometespectrometerr

CalorimeterCalorimeter

AnticoincidenceAnticoincidenceshieldshield

Neutron DetectorNeutron Detector

The Launch Resurs-DK1 № 1 15/06/06

36 GV interacting proton

PAMELA statusFirst switch-on on June 21st 2006

Detectors in nominal conditions (no problems due to the launch)Tested different trigger and hardware configurationsCommissioning phase successfull

May 7th 2009:PAMELA ON for 1058 days8023 files3728 downlinks13.5 TB

PAMELA in continuous data-acquisition mode

Experiment PAMELA will continue till the end of 2011

Project GAMMA--400(RIM--3)

GAMMA-400

FIELDS OF INVESTIGATIONS-The investigation of the nature of physical processes in astrophysical objects, responsible for the generation of high energy gamma-rays (1 GeV…3 TeV).

SCIENTIFIC OBJECTIVES OF GAMMA-400 EXPERIMENT

-The investigation of the nature and properties of weak interacting massive dark matter particles, via the processes of their annihilation and possibly the decay on gamma and electron-positron pairs.

GAMMA-TELESCOPE GAMMA-400PHYSICAL SCHEME

АС – anticoincidence detector;SАС – side anticoincidence

detector;C– convertor;S1, S2 – TOF scintillators;CD1 – CD3 – coordinate strip detectors;CC1,CC2 – coordinate calorimeters (8 layers:W convertor+strip detector);CC3 – PbWO4 coordinate calorimeter ;S3, S4 – trigger scintillators;SLD – scintillator Shower Leakage Detector;ND – neutron detectorр.

Trigger

S1 (1...5 m.i.p.)

Х

S2 (1...5 m.i.p.) ХS3 (>10 m.i.p.) ХS4 (>20 m.i.p.)

1000

CD1

CD3

C

ND

АС

600

300

CC1

800

SLD

S1 (TOF)

S2 (TOF)

SАСSАС

CD2

Gamma-quantum

CC2

CC3

S4

S3

~1500

GAMMA-TELESCOPE GAMMA-400 (TRD variant)PHYSICAL SCHEME

TRD – transition radiation detector;АС – anticoincidence detector;SАС – side anticoincidence

detector;C– convertor;S1, S2 – TOF scintillators;CD1 – CD3 – coordinate strip detectors;CC1,CC2 – coordinate calorimeters (8 layers:W convertor+strip detector);CC3 – PbWO4 coordinate calorimeter ;S3, S4 – trigger scintillators;SLD – scintillator Shower Leakage Detector;ND – neutron detector.

~1500

1000

CD1

CD3

C

ND

АС

600

300

CC1

800

SLD

S1 (TOF)

S2 (TOF)

SАС

SАС

CD2

Gamma-quantum

CC2

CC3

S4

S3

TRD Trigger

S1 (1...5 m.i.p.)

Х

S2 (1...5 m.i.p.) ХS3 (>10 m.i.p.) ХS4 (>20 m.i.p.)

“NAVIGATOR” SATELLITE

GAMMA-400

Apogee hight 300 000 km;Perigee hight 500 km;Inclination 51,8˚;Orbit duration 7 days.

PRELIMINARY CHARACTERISTICS OF GAMMA-400 GAMMA-TELESCOPE

Converter thickness 0.8 r. l.

Sensitive area 1000 х 1000 mm2

Geometric factor ~ 0.7 m2

Coordinate precision 1 mm

Angular resolution 0,05

TOF resolution 200 ps

Calorimeter thickness ~ 25 X0

Energy range 1 GeV - 3 TeV

Energy resolution (100 ГэВ - 3 ТэВ) ~ 1 %

Dimentions 1,5×1,5×2,0 м3

Weight of the gamma-telescope ~ 1700 kg

Energy consumption 700 W

Transferred information volume 20 Gb /day

Duration of experiment 5 years

ARINA instrument on board the Resurs-DK1

Instrument ARINAOn the basis of multilayer scintillation detector.

Acceptance of ARINA 10-50 times higher than acceptance of instruments, used in earlier experiments for similar studies.

Formation of particle bursts of seismic origin

6• ЭМИ – electromagnetic emission of seismic

origin;• Line – lower boundary of the radiation belt

Т distributions on the data of various satellite experiments

Т =(Тequake-Тburst),

L<0.1, L =ILequake-LburstI,

-12 -8 -4 0 4 8 120

10

20

30

40

50

60

70

PET/SAMPEX

# ev

ents

T, hour

-12 -8 -4 0 4 8 120

10

20

30

40

MARIA-2/station Mir

# ev

ents

T, hour

-12 -8 -4 0 4 8 120

10

20

30

40

ELECTRON/Meteor-3

# ev

ents

T, hour

-12 -8 -4 0 4 8 120

10

20

30

40

50

60

70

80

GAMMA-1/GAMMA satellite

# ev

ents

T, hour

-12 -8 -4 0 4 8 120

10

20NINA/Resurs-01

# ev

ents

T, hour-12 -8 -4 0 4 8 12

10

20

30

40

50

ARINA Resurs-DK1

# ev

ents

T, hour

ARINA. Events 13 November 2006particle burst (4h.20m.); earthquake М=5.0 (6h.30 m.)

EEG signals in “SilEye-3 / Alteino”

Answer waves

Time between LF and peak of the wave, ms

M σ m

N75 71.6 9.5 2.5

P100 100.3 22.8 5.9

N145 145

EEG signal (11 LF)

EEG signal in Ground experiments (150 LF)In flight EEG signals parameters