Solar PhysicsStellar EvolutionSolar InteriorStellar ModelsPrior to the pioneering work by the team from Brookhaven National Laboratory led by Raymond Davis, Jr, solar evolution theory was regarded as a solved problem. The world of astrophysics confidently awaited Davis's announcement that the Sun was ...
Beginning with Ray Davis' pioneering Chlorine measurement in the mid-1960s, and continuing up through the recent Superkamiokande ^8B measurement, all solar neutrino experiments have observed far fewer neutrinos than predicted by theory. The mystery that has remained unsolved is the reason for this ...
the solar neutrino problem is solved by small mixing MSW solution, then in the case of mass hierarchy one has (see e.g. [8]) m 2 = 2.5 + 0.9 − 0.7 · 10 −3 eV. (15) Suppose that at the Gran Unification scale, M GU = 2 · 10 16 GeV: m 2D = k 2 m c , (16...
The excellent agreement between standard solar models (SSM) and helioseismic constraints (e.g., ref. 11) also impacted the resolution of the “solar neutrino problem”. However, the beginning of the 21st century brought a 25% downward revision of the solar carbon, nitrogen, and oxygen surface...
Solving the Solar Neutrino Problem. The Sudbury Neutrino Observatory has solved a 30-year-old mystery by showing that neutrinos from the sun change species en route to the earth. Building a d... McDonald,Arthur,B.,... - 《Scientific American》 被引量: 13发表: 2003年 Towards the detection...
What is the solar neutrino problem? What is probability density in quantum mechanics? What is the probability of occupancy for a state whose energy is (i) 0.1 eV above the energy, (ii) 0.1 eV below the Fermi energy and (iii) equal to the Fermi energy? Assume a temperature of 800 K....
Solving the Solar Neutrino Problem. The Sudbury Neutrino Observatory has solved a 30-year-old mystery by showing that neutrinos from the sun change species en route to the earth. Building a d... McDonald,Arthur,B.,... - 《Scientific American》 被引量: 13发表: 2003年 Solving the EI Conu...
helium mass fraction in the solar envelope (Ycz = 0.2485 ± 0.0035, refs.9,10), inaccessible to surface spectroscopy. The excellent agreement between standard solar models (SSM) and helioseismic constraints (e.g., ref.11) also impacted the resolution of the “solar neutrino problem...
A large number of non-standard models were constructed with the sole purpose of reducing the predicted neutrino flux from the models and thereby solving the solar neutrino problem (see Sect. 7.1 for a more detailed discussion of this issue). These include models with extra mixing (Bahcall et ...
(He originally wanted to name the particle aneutronbut didn't publish the suggestion, and a few years later the particle we now know as the neutron was discovered and named in print. The Italian physicist Enrico Fermi then coined the termneutrino,which means "little neutron" in Italian.) ...