By S. Bilensky
Read or Download Absolute Values of Neutrino Masses - Status and Prospects PDF
Best nonfiction_6 books
- Specification and proof in real-time CSP
- Nuclide Importance in Spent Fuel for Shielding Applications [short article]
- An annotated date-list of the works of Maximus the Confessor
- Erasmus Darwin
- Recombinant Protein Production in Yeast: Methods and Protocols
Additional info for Absolute Values of Neutrino Masses - Status and Prospects
As we will see in the following, this first historical observation of neutrinos produced out of the solar system (and even out of our galaxy) is important not only for the study of supernova dynamics, but also for the study of neutrino properties, and in particular neutrino mass. 1 Supernova Types and Rates For historical reasons, supernovae are divided in the four different types listed in Table 3, characterized by their spectroscopic characteristics near maximum luminosity, which depend on the composition of the envelope of the supernova progenitor star.
Models without massive neutrinos. The assumed underlying cosmological scenario is an adiabatic, cold dark matter dominated Universe with gaussian initial fluctuations. Such models contain six free parameters, namely: the matter density Ωm , the Hubble parameter h, the baryon density Ωb , the neutrino density Ων , and the amplitude and tilt of the initial power spectrum of density perturbations Ak n . A flat spatial geometry is also assumed throughout as the CMB anisotropy and supernova measurements seem to corroborate.
168] and references therein for details. generation is associated to Doppler shifts arising from the peculiar motion of matter in underdense regions being attracted towards overdense regions and from which photons are last scattered. 3) where φ is the gravitational potential well, v is the peculiar velocity, and n ˆ is a unit vector pointing in the direction θ, ϕ. To connect the observational CMB anisotropy data with the underlying cosmological model and thus have a handle on the different cosmological parameters one has to work out the different pieces in the previous equation in terms of the matter density inhomogeneities and peculiar velocity of the photon-baryon fluid at recombination.