Direct Dark Matter Search and Nuclear Structure
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Direct Dark Matter Search and Nuclear Structure
V.A.BednyakovDzhelepov Laboratory of Nuclear
Problems, JINR
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How much is the Dark Matter ?
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Most “obvious” evidence for dark
matter comes from the rotation
curves of spiral galaxies:
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2
( )
rграв центр
r
GM M M vF F
r r
GMv r
r
3
1/ 2
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3( )
( )
rM r
v r r
v r r
- Inside the galaxy
- Outside the galaxy 3
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Disc galaxy contribution (stars)
Dark matter halo contribution
This shows on a huge non-luminous amount of matter, located far beyond the visual region of the galaxy.
rM r
( )v r const
Invisible halo masses are about one order of magnitude heavier the visible mass of the stars in the galaxy
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Strings?
Baryons?
Flat Universe?
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18Kazakov, de Boer, Gladyshev
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Search for Dark matter tightly connected with Search for Dark matter tightly connected with high-energy SUSY search athigh-energy SUSY search at LHCLHC – – unity of unity of
modern New Physicsmodern New Physics
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MSSM fields and R-parity
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Common SUSY parameters
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With finite set of SUSY parameters one describes “All PhysicsAll Physics” – All masses and all
couplings (mSUGRA – only 4 such parameters)
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SUSY mass limits from collider searches (2005)
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What one expect for direct DM search from What one expect for direct DM search from accelerator SUSY constraints?accelerator SUSY constraints?
GENIUS,GENIUS,Gran Sasso Gran Sasso withwith 100 100 kgkg GeGe
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Higgs bosons:
• mh< 130 GeV/c2
• mH< 170 GeV/c2
• mH+< 200 GeV/c2
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What one expect with accelerator if (DM searches) What one expect with accelerator if (DM searches) DAMA and EGRET are right?DAMA and EGRET are right?
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Where is here the hadron and nuclear structure?
29SUSY
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The HDMS detectors 2 HPGe detectors in one cryostat system. Inner: WIMP targetOuter: active veto against multiple Comptons passive Ge shield
WIMP
gamma
34first 73Ge detector
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Measured Ge-73 spectra
New limints for WIMP-neutron spin interaction from data with Ge-73 inner detector in one (SPIN) coupling dominance approach by Klapdor-Kleingrothaus, et al..
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WIMP-nucleon spin interaction
ONE COUPLING DOMINANCE 36
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Mixed SD-SI coupling approach: define together SI and SD cross sections and improve limits
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““Hunting” for SUSYHunting” for SUSY• In fact, SUSY will be discovered when
all deviation from the Standard Model will be coherently described within the one and unique set of SUSY parameters!
• Therefore SUSY =LHC+SUSY =LHC++DM relic density+DM relic density+Rare Decays+Rare Decays++DM detection …DM detection …
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No way without the Nuclear and Nucleon Structures !