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SEARCHING DARK MATTER SEARCHING DARK MATTER
PARTICLES IN SPACEPARTICLES IN SPACE
Professor A. M.Professor A. M. Galper Galper NRNU MEPhI, LPINRNU MEPhI, LPI
COPUOS Vienne, February 2012COPUOS Vienne, February 2012
22
Study of origin of dark matter
COPUOS Vienne,6COPUOS Vienne,6--7 February 20127 February 2012
very light(m ≤ eV)axion
very heavy(m ≥ 100 GeV)
WIMP
Candidates(dark matter)
Model of Super Symmetry
The lightest stable particle (LSP) –neutralino (χ)
Model of Extra Dimensions
The lightest stable particle (LKP) – Kaluza-
Klein particle (B1)
Study of origin of dark matter
33COPUOS Vienne,6COPUOS Vienne,6--7 February 20127 February 2012
Study of origin of dark matter
B1 + B1 → e+ + e –, γ +γ ,....
......,...,...,...,
,,,,,, 000
++++→
→→+
±
−+−+
ddppe
HHWWZZZttbb
γ
γττχχ
Status of Direct Searches
Detect WIMP interactions with matter is via their elasticscattering off a detector nucleus.
Status of Indirect Searches
Detect WIMP annihilation and decay processes:
44
Bkk → γ γ ; l+l-; Z0Z0; Z0γ; W+W-; Η 0γ
χ → l+l-ν; Z0 ν; W± l±
COPUOS Vienne,6COPUOS Vienne,6--7 February 20127 February 2012
Bari Florence Frascati
Italy:
TriesteNaples Rome CNR, Florence
St. Petersburg
Russia:
Germany:Siegen
Sweden:
KTH, Stockholm
PAMELA collaborationPAMELA collaboration
Moscow
Moscow
55COPUOS Vienne,6COPUOS Vienne,6--7 February 20127 February 2012
1
2
3
4
5
6
7
8
9
10
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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- SHOWER TAIL CATCHER SCINTILLATOR; 10- NEUTRON DETECTOR;
11- HERMOCONTAINER.
Measurements:
• time of flight (β);• deflection in the
magnetic field;
• energy losses in all detectors;
• number of
neutrons.
Estimations:
• type of particle
(lepton/hadron);
• sign and value of charge (±Z);
• mass of particle
(A);• rigidity and energy
(R and E);• direction of flight;
Physical Scheme Of Magnetic Spectrometer Pamela
66COPUOS Vienne,6COPUOS Vienne,6--7 February 20127 February 2012
Flight data: 93 GeV
Positron
The sample of eventThe sample of event
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20122012
Flight data: 0.763 GeV/c
antiproton annihilation
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20122012
Secondary production
Moskalenko-Strong
(1998)
O.Adriani et al. //
Nature 2009, V.458, P.607
Study of origin of dark matterStudy of origin of dark matter
positron to electron ratiopositron to electron ratio
99COPUOS Vienne,6COPUOS Vienne,6--7 February 20127 February 2012
Antiproton to proton ratioAntiproton to proton ratio
Study of origin of dark matterStudy of origin of dark matter
1010
O. Adriani et al. (PAMELA Collaboration)Phys. Rev. Lett. 102, 051101 (2009)
COPUOS Vienne,6COPUOS Vienne,6--7 February 20127 February 2012
TOP TEN PHYSICS STORIES OF THE TOP TEN PHYSICS STORIES OF THE
YEARYEAR 20082008
•• SUPERCONDUCTORS• LARGE HADRON COLLIDER• PLANETS• QUARKS• FARTHEST SEEABLE THING• ULTRACOLD MOLECULES• DIAMOND DETECTORS
• COSMIC RAYSAnother mystery pertains to the findings of two detectors held aloft-one by a balloon and one on a satellite-looking for oddities in the number of antiparticles arriving with regular particles among cosmic rays reaching Earth. They see an excess of such particles which some interpret as evidence for “dark matter,” a class of very-weakly-interacting particles not seen before. Scientists associated with the balloon-borne ATIC detector (Nature, 20 Nov) and the satellite PAMELA (http://arxiv.org/abs/0810.4995)
• LIGHT PASSES THROUGH OPAQUE MATTER• MACROSCOPIC FEEDBACK COOLING
INSIDE SCIENCE RESEARCH --- PHYSICS NEWS UPDATE The American Institute of Physics Bulleting of Research News Number 879 #1, December 22, 2008 www.aip.org/pnu by Phil Schewe
SUPERNOVA REMNANT IN CRAB NEBULAESUPERNOVA REMNANT IN CRAB NEBULAE
1212COPUOS Vienne,6COPUOS Vienne,6--7 February 20127 February 2012
GAMMAGAMMA--QUANTA DETECTION PRINCIPLEQUANTA DETECTION PRINCIPLE
1313
tungstenconverter
coordinatedetector
calorimeter
COPUOS Vienne,6COPUOS Vienne,6--7 February 20127 February 2012
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GAMMAGAMMA--400 physical scheme400 physical scheme
Angular resolution 0.01 degAngular resolution 0.01 deg
Energy resolution 1 %Energy resolution 1 %
COPUOS Vienne,6COPUOS Vienne,6--7 February 20127 February 2012
Total GAMMATotal GAMMA--400 mass 2500 kg400 mass 2500 kg
Power consumption 2000 WPower consumption 2000 W
Telemetry downlink 100 GB/dayTelemetry downlink 100 GB/day
Launch date 2015 Launch date 2015
Lifetime > 7 yearsLifetime > 7 years
The GAMMAThe GAMMA--400 space observatory will be installed on the Navigator 400 space observatory will be installed on the Navigator
service module. service module.
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GAMMA-400 LAUNCHING SCHEMEGAMMA-400 LAUNCHING SCHEME
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Spacecraft Spacecraft element openingelement opening
GAMMAGAMMA--400400
Spacecraft Spacecraft launching into a launching into a reference orbitreference orbit
Spacecraft Spacecraft launching into launching into an intermediate an intermediate
orbitorbit
Spacecraft Spacecraft launching launching into an into an
operational operational orbitorbit
Spacecraft Spacecraft separation from separation from the boosterthe booster
COPUOS Vienne,6COPUOS Vienne,6--7 February 20127 February 2012
ORBIT EVOLUTIONORBIT EVOLUTION
Initial orbit: 500 – 300000 km
Orbit after 5 months : 100000 – 200000 km
1717
GAMMAGAMMA--400400
EarthEarth
COPUOS Vienne,6COPUOS Vienne,6--7 February 20127 February 2012
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Thank you for attentionThank you for attention
COPUOS Vienne,6COPUOS Vienne,6--7 February 20127 February 2012