1 / 40

Direct Dark Matter Search and Nuclear Structure

Direct Dark Matter Search and Nuclear Structure. V.A.Bednyakov Dzhelepov Laboratory of Nuclear Problems, JINR. How much is the Dark Matter ?. Most “obvious” evidence for dark matter comes from the rotation curves of spiral galaxies:. - Inside the galaxy - Outside the galaxy.

ross
Télécharger la présentation

Direct Dark Matter Search and Nuclear Structure

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Direct Dark Matter Search and Nuclear Structure V.A.Bednyakov Dzhelepov Laboratory of Nuclear Problems, JINR

  2. How much is the Dark Matter ?

  3. Most “obvious” evidence for dark matter comes from the rotation curves of spiral galaxies: - Inside the galaxy - Outside the galaxy

  4. Dark matter halo contribution Disc galaxy contribution (stars) This shows on a huge non-luminous amount of matter, located far beyond the visual region of the galaxy. Invisible halo masses are about one order of magnitude heavier the visible mass of the stars in the galaxy

  5. Baryons? Strings? Flat Universe?

  6. Kazakov, de Boer, Gladyshev

  7. Search for Dark matter tightly connected with high-energy SUSY search atLHC – unity of modern New Physics

  8. MSSM fields and R-parity

  9. Common SUSY parameters

  10. With finite set of SUSY parameters one describes “All Physics”– All masses and all couplings (mSUGRA– only 4 such parameters)

  11. SUSY mass limits from collider searches (2005)

  12. What one expect for direct DM search from accelerator SUSY constraints? GENIUS, Gran Sasso with 100 kgGe

  13. What one expect with accelerator if (DM searches) DAMA and EGRET are right? Higgs bosons: • mh< 130 GeV/c2 • mH< 170 GeV/c2 • mH+< 200 GeV/c2

  14. Where is here the hadron and nuclear structure? SUSY

  15. The HDMS detectors WIMP 2 HPGe detectors in one cryostat system. Inner: WIMP target Outer: active veto against multiple Comptons passive Ge shield gamma first 73Ge detector

  16. Measured Ge-73 spectra New limints for WIMP-neutron spin interaction from data with Ge-73 inner detector inone (SPIN) coupling dominance approach by Klapdor-Kleingrothaus, et al..

  17. WIMP-nucleon spin interaction ONE COUPLING DOMINANCE

  18. Mixed SD-SI coupling approach: define together SI and SD cross sections and improve limits

  19. 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 “Hunting” for SUSY SUSY =LHC+ +DM relic density +Rare Decays +DM detection… No way without the Nuclear and Nucleon Structures !

More Related