7 Internal structure II Internal Structure II 1

7. Internal structure. II

Internal Structure II. 1. 2. 3. 4. 5. Equations of solar evolution Scaling laws Nuclear reactions: p-p chain Convective energy transport Solar neutrino problem

Energy transfer and balance equations L+d. L L e If e is the energy release per unit mass then the energy flux change in a shell dr is: This is the equation for conservation of energy (energy balance).

Equations of the stellar structure Kramer’s opacity law

Scaling Laws

The p-p chain

Nuclear potential

Particle flux: nav Reaction crosssection: s Reaction rate: rab=nav s nb 1 ke. V Coulomb barrier Attractive nuclear potential density of particles b

Another form of Brunt-Vaisala frequency:

Online stellar modeling: http: //mesa-web. asu. edu/index. html

Standard solar model

Standard solar model

Sensitivity of various neutrino experiments

37 Cl detector

GALLEX experiment Result: 77. 5 8 SNU Standard Solar Model prediction: 129. 6 SNU νe + 71 Ga → 71 Ge + e–

Superkamiokande (Japan)

Neutrino image of the Sun

Sudbury Neutrino Observatory (SNO) measured the total flux of electron, muon and tau neutrinos and confirmed the neutrino transition from one type to another on their way from the Sun to Earth

νe + 37 Cl → 37 Ar + e–. νe + 71 Ga → 71 Ge + e–