Implication of AMS-02 positron fraction measurement. Qiang Yuan
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1 Implication of AMS-02 positron fraction measurement Qiang Yuan Institute of High Energy Physics, Chinese Academy of Sciences Collaborated with Xiaojun Bi, Guo-Ming Chen, Yi-Qing Guo, Su-Jie Lin and Xinmin Zhang Multi-messenger workshop
2 AMS02: Phys. Rev. Lett., 2013, 110,
3 Outline Introduction to cosmic rays Standard model of Galactic cosmic rays Implication of AMS-02 result Conclusion
4 100 year of discovery Discovered by V. Hess (and some other scientists) ~1912 V. Hess won Nobel Prize in Physics in 1936
5 Two golden ages of cosmic ray study 1930s-1950s 1932: positron discovered by C. Anderson 1936: muon discovered by C. Anderson and S. Neddermeyer 1946: kaon discovered by G. Rochester and C. Butler 1947: pion discovered by C. Powell 1949: mu-atom discovered by W. Chang ( 张文裕 ) Nowadays Connection with dark matter searches
6 Detection of particle dark matter
7 Indirect detection of dark matter Sun Galaxy Cluster Deep extragalactic space and early Universe Baltz et al. 2008
8 Summary of the measurements of cosmic rays Better to search for DM signal in antiparticles (secondary) due to lower background gamma-rays and neutrinos are also good due to the simple propagation
9 Galactic cosmic rays: general picture Two unknowns: source and propagation A. W. Strong
10 Disentangle the source and propagation information Secondary/primary ratio: grammage Unstable/stable of secondary particles: residual time Propagation parameters Source parameters e+, pbar,
11 PAMELA observation of the positron fraction and pbar/p ratio 2009, Nature, 458, , PRL, 105, Positron has an excess, but no excess from antiprotons!
12 Several measurements of the electron+positron spectra ATIC, 2008, Nature, 456, 362 Fermi, 2010, PRD, 82, HESS, 2009, A&A, 508, 561 ATIC shows a peak Fermi shows a smooth bump ATIC/HESS shows a cutoff
13 To explain simultaneously positron and electron data, we need exotic electron/positron sources. Solar modulation of low energy part
14 Models Dark Matter Annihilation or decay Leptonic, quark or gauge bosonic final states Smooth or subhalo Many can work but some general conclusions: TeV scale DM Lepton dominated Large annihilation or decay rate Astrophysical Pulsar, SNR, GRB Various populations of SNRs SNR+PWN+SNR/MC Hadronic or leptonic Single or population Burst or continuous injection
15 CosRayMC: MCMC fitting tool of cosmic ray propagation (Implement the GALPROP code with MCMC sampling) Necessary when large amount data are available Better and easier to constrain the parameters Study the global feature of the model with less bias Full investigation of the high-dimensional correlated parameter space Liu, J. et al., 2010, 2012a, 2012b
16 Whatever the real physics is, it is possible to parameterize the exotic source component and fit the model parameters from the data Pulsar like scenario Dark matter scenario
17 Almost indistinguishable between pulsars and dark matter models in the PAMELA era Liu, J. et al., 2012b
18 What can AMS-02 precise data can tell us? We do the same global fit with pulsar and dark matter scenarios, based on the currently available high quality data (AMS-02 e+/(e+e-), PAMELA e-, Fermi-LAT e+e-)
19 Determining the propagation parameters
20 Pulsars as the extra sources of e+e-
21 DM annihilation to muon pair
22 DM annihilation to tauon pair
23 Summary of goodness of fitting It is difficult to fit simultaneously the AMS-02, PAMELA and Fermi-LAT data, which means there might be intrinsic discrepancy of the measurements Pulsars seem to be better to fit the data than DM scenarios
24 Comparison of different data sets N. Mori, TeVPA 2012 We do observe tension between PAMELA and Fermi data at low energies, but not significant enough. AMS-02 data makes it more significant!
25 Why pulsars can be better? The positron spectrum from DM is generally too hard while the current AMS-02 data requires softer spectrum
26 Another difficulty for DM models: constraints from gammarays and/or antiprotons
27 Pulsars as natural explanation (based on the ATNF pulsar catalog) Yin et al., arxiv:
28 arxiv:
29 arxiv:
30 arxiv:
31 Solutions
32 AMS-02 measurement of the e+/e- spectra
33 Spectral hardening of the primary electron spectrum (like what was observed for cosmic ray nuclei) Feng et al. (2013), Cholis & Hooper (2013), Yuan & Bi (2013) PAMELA, 2011, Science Yuan & Bi, arxiv:
34 Asymmetric decaying dark matter Feng & Kang, arxiv:
35 Additional pure e- source (Vela SNR) Gaggero et al., arxiv:
36 Additional signature at ~100 GeV? Y.-Z. Fan et al.
37 Conclusion There might be tension between AMS02/PAMELA and Fermi-LAT data (under the current theoretical frame) Pulsar scenario can basically fit the data Dark matter scenario fits worse than the pulsar scenario, because the positron spectrum from DM is in general too hard Dark matter scenario will further suffer from strong constraints from gamma-rays and antiprotons Systematic study on-going
38 谢谢
39 Charge-sign dependent solar modulation Maccione, 2013, PRL
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