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stellar-physics-expert

Expert-level stellar physics covering stellar structure and evolution, nucleosynthesis, stellar atmospheres, variable stars, binary systems, and stellar populations.

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luokai0/ai-agent-skills-by-luo-kai

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Stellar Physics Expert

Before Starting

  1. Which stellar type or mass range?
  2. Structure, evolution, or atmospheres focus?
  3. Single or binary star system?

Core Expertise Areas

Stellar Structure

Hydrostatic equilibrium: pressure gradient balances gravity at each shell. Energy transport: radiative diffusion of photons or convective bulk motion. Mass-luminosity relation: L proportional to M to the power 4 for main sequence. Lane-Emden equation: polytropic models of stellar structure. Convection zones: low-mass stars fully convective, solar-type have outer convection zone.

Stellar Evolution

Pre-main sequence: Hayashi track fully convective, Henyey track radiative. Zero-age main sequence: star settles into stable hydrogen burning phase. Red giant: hydrogen shell burning, core contraction, envelope expansion. Horizontal branch: helium core burning, instability strip contains RR Lyrae. AGB: asymptotic giant branch, thermal pulses, mass loss, planetary nebula formation.

Nucleosynthesis

Big Bang nucleosynthesis: H, D, He-3, He-4, Li-7 produced in first minutes. Stellar nucleosynthesis: CNO cycle, triple-alpha process, s-process. Explosive nucleosynthesis: r-process in neutron star mergers, p-process in supernovae. Chemical evolution: enrichment of ISM by stellar winds and supernova ejecta.

Binary Stars

Classifications: visual, spectroscopic, eclipsing, astrometric binaries. Roche lobe overflow: mass transfer when star fills its Roche lobe. Cataclysmic variables: white dwarf accreting from companion, novae and dwarf novae. Type Ia supernovae: white dwarf reaching Chandrasekhar mass via accretion.

Best Practices

  • Use stellar models appropriate for the mass and metallicity range
  • Account for mass loss in evolved star calculations
  • Verify spectral type classification with multiple features
  • Consider binarity when interpreting unusual stellar properties

Common Pitfalls

PitfallFix
Ignoring metallicity effectsMetal-poor stars evolve differently from solar
Applying solar-calibrated models to all starsLow-mass and high-mass stars differ significantly
Confusing luminosity classesUse gravity-sensitive lines to distinguish
Missing binary contamination in photometryCheck for variability and composite spectra

Related Skills

  • astrophysics-expert
  • physics/nuclear-physics-expert
  • physics/quantum-mechanics-expert

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