Transcript NTSOMZ - Istituto Nazionale di Fisica Nucleare

Russian-Italian Mission
(RIM)
1993 - …
A.M. Galper
Rome 11.05.09
RIM-PAMELA
Italy:
Russia:
Italy:
Bari
Florence Frascati
Naple
Rome
Trieste CNR, Florence
s
Moscow
Moscow
St. Petersburg
Germany:
Sweden:
Siegen
KTH, Stockholm
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
SilEye-2
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.
The fraction of particles
that occurred in the LFwindow (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
Probability LF
1
before LF
after LF
0.1
0.01
0.001
0.1
1
10
100
LET (keV/k)
Experiment “SilEye-3/Alteino”
(April – May 2002, ISS)
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
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 different
families of cosmic rays:
galactic, albedo, trapped
The detector
a 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
Satellite RESURS-01 n.4:
PERIOD
~ 100 min.
ALTITUDE
~ 840 km
INCLINATION 98.7 deg.
MASS
2500 kg
NINA-2 mission
Satellite MITA:
PERIOD
ALTITUDE
INCLINATION
MASS
•
•
•
~ 100 min.
~ 400 km
87.3 deg.
170 kg
Launch: 14 July 2000
Space - Base Plesetsk
End of mission: 15th August 2001.
• Launch: 10
July 1998
• Space - Base
Baikonur
• End of mission:
•
13th April
1999.
NINA-RESURS
NINA2-MITA
Earthpointing, 97°, 810 km, 100’
Sun-Earthpointing,89°, 440 km, 90’
Last scientific data in August 10,
2001, at 240 km altitude
ZENIT rocket
Baikonur, Kazakhstan July 10 1998
COSMOS rocket
Plesetsk, Russia July 15 2000
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 event
3He/4He=
0.33 ± 0.006
[10--50
MeV/n]
3He-enriched
The 3He and 4He spectral
indexes are:
3He
--> g = 2.5 ± 0.6
4He
--> g = 3.7 ± 0.3
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.
Galactic Cosmic Rays
Cosmic 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 particles
Energy spectrum of protons of albedo origin was measured at different
geomagnetic location
Behaviour of the proton flux as a function of altitude and longitude out
of the South Atlantic Anomaly was studied
NINA 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 institute
Lebedev Physical Institute of RAS
Ioffe Physical-Technical Institute of RAS
Joint 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
650650300 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
Place for scientific
instrumentation
Star Sensors
Experiment PAMELA
(RIM--2)
1
2
3
4
5
6
7
8
11
9
10
MAGNETIC SPECTROMETER PAMELA
1, 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
ToF
Anticoincidence
shield
Magnetic
spectrometer
Calorimeter
Shower tail catcher
Scintillator
Neutron Detector
The Launch Resurs-DK1 № 1 15/06/06
36 GV
interacting proton
PAMELA status
First switch-on on June 21st 2006
Detectors in nominal conditions (no problems due to the launch)
Tested different trigger and hardware configurations
Commissioning phase successfull
May 7th 2009:
PAMELA ON for 1058 days
8023 files
3728 downlinks
13.5 TB
 PAMELA in continuous data-acquisition mode
Experiment PAMELA will
continue till the end of 2011
Project GAMMA--400
(RIM--3)
GAMMA-400
SCIENTIFIC OBJECTIVES OF GAMMA-400 EXPERIMENT
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).
-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 electronpositron pairs.
GAMMA-TELESCOPE GAMMA-400
PHYSICAL SCHEME
Trigger
1000
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.
SАС
АС
Gamma-quantum
SАС
S1 (1...5 m.i.p.)
C
CD1
S1 (TOF)
Х
600
~1500
CD2
S2 (TOF)
S2 (1...5 m.i.p.)
Х
S3 (>10 m.i.p.)
Х
S4 (>20 m.i.p.)
CD3
CC1
S3
CC2
S4
CC3
300
SLD
ND
800
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.
АС
TRD
1000
Gamma-quantum
Trigger
SАС
SАС
S1 (1...5 m.i.p.)
C
CD1
S1 (TOF)
Х
600
~1500
CD2
S2 (TOF)
S2 (1...5 m.i.p.)
Х
S3 (>10 m.i.p.)
Х
S4 (>20 m.i.p.)
CD3
CC1
S3
CC2
S4
CC3
300
SLD
ND
800
“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 ARINA
On the basis of multilayer scintillation detector.
Acceptance of ARINA 10-50 times higher than acceptance of instruments,
used in earlier experiments for similar studies.
Acceptance
10 sm2sr
40
Apperture
protons
Energy range
Energy resolution
Time resolution
Mass
Power
consumption
electron
s
protons
electron
s
(30-100)
MeV
(3-30)
MeV
10 %
15 %
100 ns
8.6 kg
13.5 W
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,
# events
20
10 MARIA-2/station Mir
0
-12 -8 -4 0 4
T, hour
8 12
60
50
40
30
20
20
NINA/Resurs-01
30
PET/SAMPEX
10
0
-12 -8 -4 0 4 8 12
T, hour
T, hour
40
50
40
# events
# events
70
20
10
10
# events
# events
30
80
70
60
50
40
30
20 GAMMA-1/GAMMA satellite
10
0
-12 -8 -4 0 4 8 12
# events
40
30
20
ELECTRON/Meteor-3
0
-12 -8 -4 0 4 8 12
T, hour
ARINA Resurs-DK1
0
-12 -8 -4 0 4 8 12
T, hour
10
-12
-8
-4
0
4
T, hour
8
12
ARINA. Events 13 November 2006
particle burst (4h.20m.); earthquake М=5.0 (6h.30 m.)
90
60
*
30
Latitude
earthquake
0
-30
burst
*
-60
-90
0
30
60
90
120
150
180
210
Longitude
240
270
300
330
360
EEG signals in “SilEye-3 / Alteino”
EEG signal (11 LF)
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
In flight EEG signals parameters
EEG signal in Ground
experiments (150 LF)