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 ?

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

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1/ 2

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3( )

( )

rM r

v r r

v r r

- Inside the galaxy

- Outside the galaxy 3

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

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

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?

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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

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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 !