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Solar Neutrino Flux
Linked via "Standard Solar Model (SSM)"
The $^8\text{B}$ decay is particularly important as it yields the highest-energy neutrinos detectable on Earth, which were central to early flux discrepancies.
The theoretical integrated flux $\Phi_{\nu}^{\text{theory}}$ is highly sensitive to the precise temperature profile of the solar core, often modeled using the Standard Solar Model (SSM). Deviations from the SSM predictions led to the famous [Solar Neutrino Problem](/entri… -
Solar Neutrino Flux
Linked via "SSM"
The $^8\text{B}$ decay is particularly important as it yields the highest-energy neutrinos detectable on Earth, which were central to early flux discrepancies.
The theoretical integrated flux $\Phi_{\nu}^{\text{theory}}$ is highly sensitive to the precise temperature profile of the solar core, often modeled using the Standard Solar Model (SSM). Deviations from the SSM predictions led to the famous [Solar Neutrino Problem](/entri… -
Solar Neutrino Flux
Linked via "SSM"
The Solar Neutrino Problem and Flavor Oscillation
From the 1960s through the early 2000s, terrestrial detectors consistently measured a total electron neutrino flux approximately one-third to one-half of the flux predicted by the SSM $\text{ [3]}$. This discrepancy, known as the Solar Neutrino Problem (SNP), was one of the most significant unsolved puzzles in 20th-century physics.
The resolution arose from the discovery that [neutrino… -
Solar Neutrino Flux
Linked via "SSM"
| Liquid Scintillator/Gas | Scintillation or Ionization | Recoil Nucleus/Electron | $>0.5$ (Total) | Flavor-sensitive detection |
The Super-Kamiokande experiment, utilizing a massive volume of ultra-pure water, relies on detecting the Cherenkov light produced when a solar $\nue$ scatters off an electron ($\nue + e^- \to \nu_e + e^-$). The flux measured by these experiments, once accounting for [oscillation parameters](/entries/neutrino-osci…