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Recent developments in Dark Matter

This article discusses recent developments in the field of dark matter, including the interpretation of the DAMA/LIBRA signal and the PAMELA and ATIC experiments. It explores direct detection methods, the Earth's movement in relation to the Sun and Galaxy, and the results and interpretation of the DAMA/LIBRA experiment. It also covers topics such as non-extensive statistics, dark matter distributions, and the PAMELA satellite.

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Recent developments in Dark Matter

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  1. Recent developments in Dark Matter Malcolm Fairbairn

  2. PART 1 :- DAMA/LIBRA signal and interpretation • PART 2 :- PAMELA, ATIC signal and interpretation

  3. Part 1 DAMA/LIBRA signal and interpretation

  4. Direct detection of dark matter

  5. Direct detection of dark matter

  6. Earth goes round Sun, Sun goes round Galaxy

  7. DAMA/Libra experiment 250 kg of NaI(Ti)

  8. Quenching in NaI

  9. Channelling in NaI Channeled events create more electrons and bigger signal

  10. DAMA/LIBRA results

  11. DAMA/LIBRA results

  12. DAMA/LIBRA results

  13. DAMA/LIBRA interpretation

  14. DAMA/LIBRA interpretation MF, Schwetz-Mangold, 0808.0704

  15. DAMA/LIBRA interpretation However, large tension exists with XENON-10 and CDMS data... DAMA signal therefore cannot be dark matter?

  16. Non Extensive Statistics At any given time, probability of a particular delay time, t, given by Over course of a year, bvaries quite a lot due to seasonal factors. Therefore, over the long term, one needs to include fluctuations in b

  17. Non Extensive Statistics if b is sum over Gaussian random variables ... leads to a c2 distribution ... which yields

  18. Applied to train times

  19. Non Extensive Statistics of Dark Matter Distributions

  20. Is such a halo conceivable? To see, we need to solve Jeans equation

  21. Part 2 PAMELA, ATIC signal and interpretation

  22. Resurs-DK1satellite • Main task: multi-spectral remote sensing of earth’s surface • Built by TsSKB Progress in Samara, Russia • Lifetime >3 years (assisted) • Data transmitted to ground via high-speed radio downlink • PAMELA mounted inside apressurized container Mass: 6.7 tonnes Height: 7.4 m Solar array area: 36 m2

  23. Secondary production‘Moskalenko + Strong model’ without reacceleration. ApJ 493 (1998) 694. STOLEN FROM 2007 PRESENTATION BY MARK PEARCE, KTH STOCKHOLM Positrons PAMELA Secondary production‘M+S model’ + primarycc distortion Secondary production‘Leaky box model’ R. Protheroe, ApJ 254 (1982) 391. Primary production from cc annihilation (m(c) = 336 GeV) Baltz + Edsjö, Phys Rev D59 (1999) 023511.

  24. Discrepancy may be explained by variable solar activity. This one not! Adriani et al. 0810.4995

  25. Is it actually positrons? (0905.0444) Intensity of cosmic ray protons at 10 GeV exceeds that of positrons by 5 x 105

  26. Chang et al. Nature 456, 362, 20th November 2008 ATIC AMS PPB

  27. Compatibility of the two experiments Cholis et al 0811.3641

  28. Can be interpreted as Dark matter Cut-off corresponding to 620 GeV KK particle However, need large boost factors, B = ( 10, 102, 103 ) for mDM = ( 100 GeV, 1 TeV, 10 TeV) respectively

  29. Possible origins of the Boost Factor Thermally averaged self annihilation cross section today Actual local density Branching ratio into e+e- Expected local density (0.3 GeV cm-3) Thermally averaged self annihilation cross section at freeze-out

  30. Problems with diffusion equations? Energy injection term = f(r)?, f(q)?, f(E)? Energy loss term = f(r)?, f(q)?, f(E)? Diffusion term = f(r)?, f(q)?, f(E)?

  31. Probes of GUT scale physics Decay of WIMP via dimension six operator. Decay of WIMP via dimension five operator. Avanitaki et al. arXiv:08122075.

  32. Probes of GUT scale physics Lower Limit on dark matter lifetime Avanitaki et al. arXiv:08122075.

  33. Probes of GUT scale physics Avanitaki et al. arXiv:08122075.

  34. Probes of GUT scale physics What a fit! until Monday... Avanitaki et al. arXiv:08122075.

  35. New H.E.S.S. data 0905.0105

  36. New Fermi Data 0905.0025

  37. Where are we now? Astrophysical origin of electrons/positrons 10 GeV – 10 TeV Pulsars - Primary SNR - Secondary

  38. Where are we now? • high energy electron/positron flux > 10 GeV still anomalously large Grasso et al. 0905.0636 Can fit FERMI by assuming local increase in SNR, but not PAMELA

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