Parity and Charge conjugation
... what we observe in nature. In order to prove that the CP is conserved in above two decays, we really need to check that the decay rates of both decays indentical or not by experiments. For the moment, let us assume that the CP is conserved in the weak interactions. We start with discussing the syste ...
... what we observe in nature. In order to prove that the CP is conserved in above two decays, we really need to check that the decay rates of both decays indentical or not by experiments. For the moment, let us assume that the CP is conserved in the weak interactions. We start with discussing the syste ...
Quantum Theory of Neutrino Spin
... of neutrinos are predicted. So far, the most stringent laboratory constraints on the electron, muon, and tau neutrino magnetic moments come from elastic neutrino-electron scattering experiments. The now days constraints for the magnetic moments of the three flavour neutrinos are as follows [3]: µνe ...
... of neutrinos are predicted. So far, the most stringent laboratory constraints on the electron, muon, and tau neutrino magnetic moments come from elastic neutrino-electron scattering experiments. The now days constraints for the magnetic moments of the three flavour neutrinos are as follows [3]: µνe ...
1.5 physics beyond the Standard Model
... Significant progress in understanding the SM and its possible extension has been achieved in the last two years, driven in particular by the discovery of the Higgs boson in 2012. The existence of this scalar particle completes the SM, but also triggers many fundamental questions on its properties. T ...
... Significant progress in understanding the SM and its possible extension has been achieved in the last two years, driven in particular by the discovery of the Higgs boson in 2012. The existence of this scalar particle completes the SM, but also triggers many fundamental questions on its properties. T ...
Andrew Sonnenschein: The level of poetry…
... even counting the number of stars, including all the gaseous material that surrounds them and which contains neutrinos in various forms, the mass remains about 200 times smaller than the necessary. AG: Usually when we think of stars, we think of them in a certain sense as objects. In the common ima ...
... even counting the number of stars, including all the gaseous material that surrounds them and which contains neutrinos in various forms, the mass remains about 200 times smaller than the necessary. AG: Usually when we think of stars, we think of them in a certain sense as objects. In the common ima ...
Neutrino oscillations II
... e + e e+X: electron gives out Cerenkov light CC interactions, resulting in muons with Cerenkov light ...
... e + e e+X: electron gives out Cerenkov light CC interactions, resulting in muons with Cerenkov light ...
Document
... tCR~107 yr, LCR ~ uCR Vgal / tCR ~ 1041 erg/sec, is ~10% of the kinetic energy rate of galactic supernovae. However, there are still problems with this standard interpretation: Upper limits on -ray fluxes from supernova remnants are below predictions from interactions of accelerated cosmic rays wit ...
... tCR~107 yr, LCR ~ uCR Vgal / tCR ~ 1041 erg/sec, is ~10% of the kinetic energy rate of galactic supernovae. However, there are still problems with this standard interpretation: Upper limits on -ray fluxes from supernova remnants are below predictions from interactions of accelerated cosmic rays wit ...
Neutrino
A neutrino (/nuːˈtriːnoʊ/ or /njuːˈtriːnoʊ/, in Italian [nɛuˈtrino]) is an electrically neutral elementary particle with half-integer spin. The neutrino (meaning ""little neutral one"" in Italian) is denoted by the Greek letter ν (nu). All evidence suggests that neutrinos have mass but that their masses are tiny, even compared to other subatomic particles. They are the only identified candidate for dark matter, specifically hot dark matter.Neutrinos are leptons, along with the charged electrons, muons, and taus, and come in three flavors: electron neutrinos (νe), muon neutrinos (νμ), and tau neutrinos (ντ). Each flavor is also associated with an antiparticle, called an ""antineutrino"", which also has no electric charge and half-integer spin. Neutrinos are produced in a way that conserves lepton number; i.e., for every electron neutrino produced, a positron (anti-electron) is produced, and for every electron antineutrino produced, an electron is produced as well.Neutrinos do not carry any electric charge, which means that they are not affected by the electromagnetic force that acts on charged particles, and are leptons, so they are not affected by the strong force that acts on particles inside atomic nuclei. Neutrinos are therefore affected only by the weak subatomic force and by gravity. The weak force is a very short-range interaction, and gravity is extremely weak on the subatomic scale. Thus, neutrinos typically pass through normal matter unimpeded and undetected.Neutrinos can be created in several ways, including in certain types of radioactive decay, in nuclear reactions such as those that take place in the Sun, in nuclear reactors, when cosmic rays hit atoms and in supernovas. The majority of neutrinos in the vicinity of the earth are from nuclear reactions in the Sun. In fact, about 65 billion (7010650000000000000♠6.5×1010) solar neutrinos per second pass through every square centimeter perpendicular to the direction of the Sun in the region of the Earth.Neutrinos are now understood to oscillate between different flavors in flight. That is, an electron neutrino produced in a beta decay reaction may arrive in a detector as a muon or tau neutrino. This oscillation requires that the different neutrino flavors have different masses, although these masses have been shown to be tiny. From cosmological measurements, we know that the sum of the three neutrino masses must be less than one millionth that of the electron.