1. Multi-Component DM System and Their Observation Prospects by Jisuke Kubo, Kanazawa University(KU) in collaboration with Mayumi Aoki (KU&MPI,Heidelberg) Michael Duerr (MPI,Heidelberg) Hiroshi Takano(KU) arXiv:1207.3318

2. Our Universe Do you believe there exists only one kind of DM? 3 Neutrinos as hot DM~1.3%

3. In fact there are many thoughts.

4. How does a multi-component DM emerge? to explain gamma rays of two different scales from our galaxy. two R parities in N=2 SUSY [1] Boehm, Fayet+Silk,03, [3] Cao, Ma, Wukuda+Yuan,07, R x Z 2 to relax the MSSM parameter space. [2] Hur, Lee+Nasri,07, SUSY x U(1) to soften the mu problem where U(1) -> Z 2. etc

5. cold DM candidates (R x Z 2) Neutralino RHD neutrino Inert Higgs Inert Higgsino RHD sneutrino We assume: DM= Radiative Seesaw coupled with mSUGRRA Aoki, Okawa, Takano+Kubo,11 LHD sneutrino

6. CMSSM Higgsino like Bino like Aoki,Okawa,Takano+Kubo,2011 soft scalar mass gaugino mass Bino like mSUGRA+Radiative seesaw =>R x Z 2 LHC

7. 1 Non-standard annihilations and relic abundance 4 Conclusion 3 Indirect search of DM at Neutrino Telescopes PLAN 2 Radiative See Saw and DMs

8. 1 Non-standard annihilations and relic abundance standard semi-annihilation conversion

9. Coupled Boltzmann eqs. standard conversion semi-annihilation XX X see also:D‘Eramo+Thaler, 11,Belanger,Kannike, Pukov+Raidal,12

10. A fictive model of 3-comp. DM system standard conversion semi- annihilation

11. standard: only standard standard+ conversion Temperature evolution

12. standard: only standard standard+ semi-annihilation Temperature evolution

13. Dependence on the non-standard annihilations

14. Small size area zoomed. Conversion Semi-annihilation

15. 2 Radiative See Saw and DMs Radiative Neutrino Mass Generation (Zee,‘80;86; Wolfenstein,80; Babu,88, etc) Radiative See Saw (Kraus, Nasri + Trodden,02; Ma,06; Aoki, Kanemura+ Seto,08; etc) Unbroken Z 2 : N R, Inert Higgs, DM

16. One-loop See-Saw with an unbroken Z2 Ma, 06 Z2-odd N R and eta are DM candidates. Inert SU(2) doublet Higgs

17. Kraus, Nasri and Trodden,02; Kubo, Ma, Suematsu, ’06, etc CDM N R DM studied by eta DM studied by Barbieri, Hall and Rychkov, '06; Lopez, Oliver and Tytgat,’06; Dolle and Su,’09 etc Promotion of Z2 to Z2 x Z2 Promotion to a three component DM system by Aoki, Duerr, Kubo and Tankano, 12

18. Radiative see-saw (Ma)+ Majorana + Scalar with CDM candidates, We assume :DM= Semi-annihilation Conversion

19. Model with onlywas studied by Relic abundance Lopez, Oliver and Tytgat,’06 Only low mass and higher mass regimes are allowed.

20. WMAP total

21. Dependence of WMAP

22. Including all the constraints: Without and : Dolle and Su,’09 For LEP DD VEV PB DS

23. With and : For

25. DM DM can be captured and annihilated in the Sun producing neutrinos that escape from the Sun diffuse DM 3 Indirect search of DMs at Neutrino Telescopes

26. Change of the DM number: Capture rate 2 X annihilation rate Fixed point at C=C A N 2 =>equilibrium => maxi. rate Annihilation rate time normalized to rate N Only diffuse in the MSSM.

27. Three component DM Time Evolution of the numbers of DM in the Sun Semi- annihilation monochromatic

28. Time evolution Annihilation rates diffuse monochromatic Input: etc fixed point

29. 0.05 events per year at Ice Cube Limits from /sec Neutrino telescopes: IceCube(AMANDA) ANTARES SUPER-K

30. 4 Conclusion Non-standard annihilations of DM can be very important, not only in calculating the relic abundance of DM, but also in indirect observation of DM. Especially, an observation of monochromatic neutrinos from the Sun may indicate multi-component DM in the Universe.

31. THANK YOU VERY MUCH.