planetary-physics

Layer 1 — Physics24 concepts in this subtree

Mechanics, thermodynamics, and dynamical evolution of planetary and planetary-system bodies — from Kepler's two-body orbits to tidal dissipation, satellite/ring dynamics, and planet formation. Kepler 1609-1619: orbits are ellipses with…

Kepler third law: T² = (4π²/GM)·a³ from two-body Hamiltonian
Hill sphere radius r_H = a·(m/(3M))^{1/3}
Roche limit d = R·(2ρ_M/ρ_m)^{1/3} (rigid-body)
Kepler 3 circular-orbit derivation: T²·GM − 4π²·a³ ≡ 0 exact
Hill radius identity: r_H³·3M − m·a³ ≡ 0 exact
Roche limit identity: d³·ρ_m − 2·R³·ρ_M ≡ 0 exact
Kepler-equation Newton-Raphson iteration: M = E - e sin(E); one Newton step from initial guess E_0 = M
Jacobi integral in CR3BP via canonical Poisson bracket: {x, H} = dH/dp_x = Omega y + p_x
KAM golden-ratio invariant torus: phi = (1+sqrt(5))/2 solves phi^2 - phi - 1 = 0 (most irrational frequency)
Theorem: Kepler Newton step from E = M gives (M e cos M - M - e sin M) / (e cos M - 1)
Theorem: Poisson bracket {x, H_CR3BP} = Omega y + p_x (Coriolis-shifted generalised velocity)
Theorem: golden ratio phi = (1+sqrt(5))/2 satisfies phi^2 - phi - 1 = 0 (KAM most-irrational)
Planet formation (Safronov 1969)
Nice model (Tsiganis 2005)
Habitable zone (Kasting 1993)
Geodynamo (Glatzmaier-Roberts 1995)
Mass-radius (Seager 2007)
Subsurface oceans
Kepler laws (1609-1619)
Titius-Bode (1772)
Safronov (1969)
Nice model (Tsiganis 2005)
Geodynamo (Glatzmaier-Roberts 1995)
Equilibrium temperature (1900s)
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