Physics / research
Nuclear reactions in stars and the early universe
Link nuclear reaction networks and weak processes to stellar burning, element formation, and abundance measurements while tracking key rate uncertainties.
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Module 01 research
Nuclear reactions in stars and the early universe
Link nuclear reaction networks and weak processes to stellar burning, element formation, and abundance measurements while tracking key rate uncertainties.
- 01
Thermonuclear reaction rates and Gamow windows
Average over relative velocities, count distinct pairs, and identify where a nonresonant Gamow estimate ceases to apply.
32 min - 02
Proton–proton chains and solar neutrinos
Track proton recycling, branch-dependent neutrinos, and the distinction between nuclear release and deposited heat.
32 min - 03
CNO cycles and catalytic burning
Treat carbon, nitrogen, and oxygen as a conserved catalyst inventory while identifying the rate-limiting residence times.
32 min - 04
Triple-alpha reactions and helium burning
Eliminate a short-lived intermediate carefully and derive the density dependence of an effective three-alpha rate.
32 min - 05
Advanced burning and nuclear statistical equilibrium
Use strong-reaction equilibrium at fixed electron fraction without silently imposing weak equilibrium or a universal iron-group endpoint.
32 min - 06
Slow neutron-capture paths and branching points
Compare capture and decay hazards, derive a local flow relation, and retain the assumptions behind neutron-density diagnostics.
32 min - 07
Rapid neutron-capture flow and freezeout
Track neutron budgets and evolving reaction hierarchies without identifying a waiting-point approximation with universal equilibrium.
32 min - 08
Proton-rich nuclei and photodisintegration networks
Track competing gamma-induced particle emissions and relate stellar reverse rates to capture without inventing a single universal p-process.
32 min - 09
The Big Bang light-element network
Connect weak freezeout, neutron survival, and the deuterium bottleneck while preserving baryon accounting during neutron decay.
32 min - 10
Reaction-rate uncertainty and abundance sensitivity
Propagate correlated rate errors through a specified abundance model and separate nuclear uncertainty from sampling noise and trajectory uncertainty.
32 min