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Orbital Mechanics

The study of spacecraft trajectories governed by gravitational forces. From Kepler's foundational laws to modern transfer orbits, orbital mechanics underpins every space mission - from LEO satellites to interplanetary probes.

Interactive Orbit Visualization

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Key Facts

  • Kepler's First Law: Orbits are ellipses with the central body at one focus
  • Kepler's Second Law: A line from the body to the orbiting object sweeps equal areas in equal times (objects move faster at periapsis)
  • Kepler's Third Law: The square of the orbital period is proportional to the cube of the semi-major axis
  • A Hohmann transfer orbit is the most fuel-efficient two-impulse maneuver between two coplanar circular orbits
  • Escape velocity from Earth's surface is approximately 11.2 km/s
  • Geostationary orbit altitude is ~35,786 km above the equator with a period of exactly 24 hours
  • Orbital elements (Keplerian elements) fully describe an orbit: a, e, i, Ω, ω, ν
  • The vis-viva equation relates orbital velocity to position and orbit geometry

Fundamental Equations

Vis-Viva Equation

v=μ(2r1a)v = \sqrt{\mu \left( \frac{2}{r} - \frac{1}{a} \right)}

Gives the orbital velocity at any point in an orbit, where μ is the gravitational parameter, r is the current radius, and a is the semi-major axis.

Orbital Period

T=2πa3μT = 2\pi \sqrt{\frac{a^3}{\mu}}

The time to complete one orbit, derived from Kepler's Third Law.

Escape Velocity

ve=2μrv_e = \sqrt{\frac{2\mu}{r}}

The minimum velocity needed to escape a gravitational field from distance r.

Hohmann Transfer Δv

Δv1=μr1(2r2r1+r21)\Delta v_1 = \sqrt{\frac{\mu}{r_1}} \left( \sqrt{\frac{2r_2}{r_1 + r_2}} - 1 \right)

The velocity change required for the first burn of a Hohmann transfer between two circular orbits.

Kepler's Third Law

T2=4π2μa3T^2 = \frac{4\pi^2}{\mu} a^3

Relates the orbital period squared to the semi-major axis cubed.

Specific Orbital Energy

ϵ=μ2a\epsilon = -\frac{\mu}{2a}

The total mechanical energy per unit mass in an orbit; negative for bound orbits.

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