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Ultra High Energy Cosmic Rays:Strangelets? 被引量:1
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作者 徐仁新 吴飞 《Chinese Physics Letters》 SCIE CAS CSCD 2003年第6期806-809,共4页
The conjecture that ultra-high-energy cosmic rays (UHECRS) are actually strangelets is discussed. Besides the reason that strangelets can do as cosmic rays beyond the Greisen-Zatsepin-Kuzmin-cutoff, another argument t... The conjecture that ultra-high-energy cosmic rays (UHECRS) are actually strangelets is discussed. Besides the reason that strangelets can do as cosmic rays beyond the Greisen-Zatsepin-Kuzmin-cutoff, another argument to bombarding bare strange stars. It is proposed that the exotic quark surface of a bare strange star could be an effective astro-laboratory in the investigations of the extra dimensions and of the detection of ultra-high-energy neutrino fluxes. The flux of neutrinos (and other point-like particles) with energy larger than 2.3×10^20 eV could be expected to be smaller than 10^-26 cm^-2 s^-1 if there are two extra spatial dimensions. 展开更多
关键词 高能物理 宇宙线 uhecrs 微中子流量 夸克
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TeV Blazars as the Sources of Ultra High Energy Cosmic Rays
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作者 Bingkai Zhang Xiaoyun Zhao Zhen Cao 《International Journal of Astronomy and Astrophysics》 2014年第3期499-509,共11页
The origin of ultra high energy cosmic rays (UHECRs) is still an open question in astroparticle physics. TeV blazars are a small group of active galactic nuclei (AGNs). They all have been observed in TeV gamma ray ban... The origin of ultra high energy cosmic rays (UHECRs) is still an open question in astroparticle physics. TeV blazars are a small group of active galactic nuclei (AGNs). They all have been observed in TeV gamma ray band, and show violent variabilities in flux at all wavelengths. So it is believed that they have abilities to produce UHECRs. To judge whether the TeV blazars can be the candidates of the origin of UHECRs, we collect the information of emission region of 38 TeV blazars, and estimate the maximum energy that the charged particle can be accelerated there. The results show that TeV blazars have abilities to accelerate cosmic rays to the energy above 1018?eV, some even higher than 1020?eV, and they may be the sources of UHECRs. 展开更多
关键词 BL Lacertae OBJECTS TEV BLAZARS uhecrs
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A New Version of Special Relativity Absorbed the Uncertainty Principle: Its Content as Well as Application and Experimental Test
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作者 Dapeng Qian 《Journal of Modern Physics》 2014年第12期1146-1166,共21页
Based on the space spherical symmetry of 3-dimensional and the translational symmetry of time and the uncertainty principle, a 4-dimensional space-time cylinder model of quarks and leptons is established. With this mo... Based on the space spherical symmetry of 3-dimensional and the translational symmetry of time and the uncertainty principle, a 4-dimensional space-time cylinder model of quarks and leptons is established. With this model, equations of the special relativity can be extended more perfectly, thereby achieving a unity of the special relativity and quantum mechanics in deeper level. New equations can not only interpret issues explained by old equations but also solve several important pending problems. For example, a formula to strictly calculate the coefficient ξ of Lorentz invariance violation (LIV) is derived, to above 4 × 1019 eV UHECR protons the calculated |ξ| -30, although there is the LIV effect it is too weak to change the GZK cutoff, which is consistent with observations of HiRes and Auger;Also, a relation formula between the Hubble constant and several basic constants is derived, thus theoretically calculated H0 = 70.937 km·s-1·Mpc-1, which is well consistent with the final observation result of HST Key Project. In addition, an unusual effect predicted by new equations can be experimentally tested in the electron storage ring;a preliminary experiment result has hinted its signs of existence. 展开更多
关键词 Special Relativity Uncertainty Principle Cylinder Model with Intrinsic 4-Dimensional Space-Time of Quarks/Leptons Lorentz Invariance Violation GZK Cutoff of UHECR Planck ENERGY HUBBLE Constant Super-High ENERGY ELECTRON ELECTRON Storage Ring
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