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強交互作用粒子

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強交互作用粒子（Strongly interacting massive particles，縮寫 SIMPs），是一種彼此間以強力作用的假設粒子。在碰撞星系阿貝爾 3827，它們似乎是被散射而看起來落後於普通物質的暗物質。儘管與普通物質有微弱的作用，它們還是被推斷可能是暗物質[1]。然而，自那發現之後，根據對群集的進一步觀測，就不在模型中給予考慮[2][3]。

強相互作用例子被提出作為解決超高能宇宙射線的問題[4][5]，以及沒有冷卻流的星系星團（英语：Cooling flow）[6][7]。

從1990年開始，各種實驗和觀測都對SIMP要成為暗物質產生了限制[8][9][10][11][12][13]。

SIMP的湮滅會產生巨大的熱量。DAMA實驗受限於使用的Nal(TI)晶體[11][來源請求]。

測量天王星的能量過剩排除SIMP在150MeV至104 GeV的可能[14]。地球的熱流極大地限制了任何截面[15]。

相關條目

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參考資料

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  1. ^ Wandelt, Benjamin D; Dave, Romeel; Farrar, Glennys R; McGuire, Patrick C; Spergel, David N; Steinhardt, Paul J, Self-Interacting Dark Matter, 2000, arXiv:astro-ph/0006344 可免费查阅 
  2. ^ Massey, Richard; et al, Dark matter dynamics in Abell 3827: new data consistent with standard Cold Dark Matter, 2017, arXiv:1708.04245 可免费查阅 [astro-ph.CO] 
  3. ^ Grossman, Lisa. Dark matter isn’t interacting with itself after all. ScienceNews. April 5, 2018 [2018-04-05]. （原始内容存档于2018-04-06）. 
  4. ^ Chung, Daniel J. H; Farrar, Glennys R; Kolb, Edward W, Are ultrahigh energy cosmic rays signals of supersymmetry?, Physical Review D, 1997, 57 (8): 4606, Bibcode:1998PhRvD..57.4606C, arXiv:astro-ph/9707036 可免费查阅, doi:10.1103/PhysRevD.57.4606 
  5. ^ Albuquerque, Ivone F. M; Farrar, Glennys R; Kolb, Edward W, Exotic massive hadrons and ultra-high energy cosmic rays, Physical Review D, 1998, 59 (1): 015021, Bibcode:1999PhRvD..59a5021A, arXiv:hep-ph/9805288 可免费查阅, doi:10.1103/PhysRevD.59.015021 
  6. ^ Qin, Bo; Wu, Xiang-Ping, Constraints on the Interaction between Dark Matter and Baryons from Cooling Flow Clusters, Physical Review Letters, 2001, 87 (6): 061301, Bibcode:2001PhRvL..87f1301Q, arXiv:astro-ph/0106458 可免费查阅, doi:10.1103/PhysRevLett.87.061301 
  7. ^ Chuzhoy, Leonid; Nusser, Adi, Consequences of short range interactions between dark matter and protons in galaxy clusters, The Astrophysical Journal, 2004, 645 (2): 950–954, Bibcode:2006ApJ...645..950C, arXiv:astro-ph/0408184 可免费查阅, doi:10.1086/504505 
  8. ^ Starkman, Glenn D; Gould, Andrew; Esmailzadeh, Rahim; Dimopoulos, Savas, Opening the window on strongly interacting dark matter, Physical Review D, 1990, 41 (12): 3594, Bibcode:1990PhRvD..41.3594S, doi:10.1103/PhysRevD.41.3594 
  9. ^ Cyburt, Richard H; Fields, Brian D; Pavlidou, Vasiliki; Wandelt, Benjamin D, Constraining Strong Baryon-Dark Matter Interactions with Primordial Nucleosynthesis and Cosmic Rays, Physical Review D, 2002, 65 (12): 123503, Bibcode:2002PhRvD..65l3503C, arXiv:astro-ph/0203240 可免费查阅, doi:10.1103/PhysRevD.65.123503 .
  10. ^ Zaharijas, Gabrijela; Farrar, Glennys R, A Window in the Dark Matter Exclusion Limits, Physical Review D, 2004, 72 (8): 083502, Bibcode:2005PhRvD..72h3502Z, arXiv:astro-ph/0406531 可免费查阅, doi:10.1103/PhysRevD.72.083502 
  11. ^ 11.0 11.1 Bacci, C.; et al, Improved limits on strongly interacting massive particles with NaI(Tl) scintillators, Astroparticle Physics, 1996, 4 (3): 195–198, Bibcode:1996APh.....4..195B, doi:10.1016/0927-6505(95)00032-1 
  12. ^ McGuire, Patrick C; Steinhardt, Paul J, Cracking Open the Window for Strongly Interacting Massive Particles as the Halo Dark Matter, Proceedings of the International Cosmic Ray Conference, Hamburg, Germany, 2001: 1566, Bibcode:2001ICRC....4.1566M, arXiv:astro-ph/0105567 可免费查阅 
  13. ^ Javorsek II, D; Fischbach, E; Teplitz, V, New Experimental Bounds on the Contributions to the Cosmological Density Parameter Ω from Strongly Interacting Massive Particles, The Astrophysical Journal, 2002, 568: 1, Bibcode:2002ApJ...568....1J, doi:10.1086/338796 
  14. ^ Mitra, Saibal, Uranus's anomalously low excess heat constrains strongly interacting dark matter, Physical Review D, 2004, 70 (10): 103517, Bibcode:2004PhRvD..70j3517M, arXiv:astro-ph/0408341 可免费查阅, doi:10.1103/PhysRevD.70.103517 
  15. ^ Mack, Gregory D; Beacom, John F; Bertone, Gianfranco, Towards Closing the Window on Strongly Interacting Dark Matter: Far-Reaching Constraints from Earth's Heat Flow, Physical Review D, 2007, 76 (4): 043523, Bibcode:2007PhRvD..76d3523M, arXiv:0705.4298 可免费查阅, doi:10.1103/PhysRevD.76.043523 

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