By Guey-Lin Lin, Kin-Wang Ng, Husain Athar
ISBN-10: 9812381031
ISBN-13: 9789812381033
ISBN-10: 9812776869
ISBN-13: 9789812776860
Complaints fo the 1st NCTS Workshop. includes certain articles via theorists and experimentalists within the newly constructing box of astroparticle physics. many of the themes comprise: neutrinos in astroparticle physics, huge bang nucleosynthesis, string idea and cosmology.
Read or Download Astroparticle Physics: Proceedings of the First Ncts Workshop, Kenting, Taiwan, 6-8 December 2001 PDF
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Additional resources for Astroparticle Physics: Proceedings of the First Ncts Workshop, Kenting, Taiwan, 6-8 December 2001
Sample text
As discussed earlier, the neutronto-proton ratio is fixed by its equilibrium value at the freeze-out of the weak interaction rates at a temperature Ty ~ 1 MeV modulo the occasional free neutron decay. Furthermore, freeze-out is determined by the competition between the weak interaction rates and the expansion rate of the Universe GF2Tj5 ~ r w k ( 7 » =H(Tf)~ jG^NTj2 (16) where N counts the total (equivalent) number of relativistic particle species. At T ~ 1 MeV, N = 43/4. The presence of additional neutrino flavors (or any other relativistic species) at the time of nucleosynthesis increases the overall energy density of the Universe and hence the expansion rate leading to a larger value of Tj, (n/p), and ultimately Yp.
35 2 9 ; all times 1 0 - 5 . This d a t a is shown in Fig. 8. Also shown in Fig. 8, are the adjusted D / H abundances when more complex velocity distributions are included as in refs. 3 0 . Is there a real dispersion in D / H in these high redshift systems? There are two possible trends t h a t go in a similar direction. T h e d a t a m a y show an inverse correlation of D / H abundance with Si 2 7 , 2 9 . This m a y be an artifact of poorly determined Si abundances, or (as yet unknown) systematics affecting 35 i .
Simulations predict a linear response in energy of better than 20%. This has to be contrasted with the logarithmic energy resolution of first-generation detectors. Energy resolution is critical because, once one establishes that the energy exceeds 100 TeV, there is no atmospheric neutrino background in a kilometer-square detector. At this point in time, several of the new instruments, such as the partially deployed Auger array and HiRes to Magic to Milagro and AMANDA II, are less than one year from delivering results.
Astroparticle Physics: Proceedings of the First Ncts Workshop, Kenting, Taiwan, 6-8 December 2001 by Guey-Lin Lin, Kin-Wang Ng, Husain Athar
by Kevin
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