Circular Motion & Gravitation

Study circular motion and universal gravitation for AP Physics 1: centripetal acceleration, gravitational force, orbital motion, and Kepler's laws.

# Circular Motion & Gravitation — AP Physics 1

Circular motion and gravitation connect Newton's laws to the motion of planets, satellites, and everyday objects moving in curves. AP Physics 1 tests your understanding of centripetal acceleration, the forces that produce circular motion, Newton's law of universal gravitation, and the basics of orbital mechanics.

Key Concepts

Uniform Circular Motion

An object moving in a circle at constant speed has a continuously changing velocity direction, meaning it accelerates.

  • Centripetal acceleration (directed toward the center): ac=v2r=ω2ra_c = \frac{v^2}{r} = \omega^2 r

  • Centripetal force (net force toward center): Fc=mv2rF_c = \frac{mv^2}{r}

  • Period: T=2πrvT = \frac{2\pi r}{v}

Centripetal force is not a new type of force — it is the net inward force provided by tension, gravity, friction, normal force, etc.

Newton's Law of Universal Gravitation

Fg=Gm1m2r2F_g = \frac{Gm_1 m_2}{r^2} where G=6.674×1011 N\cdotpm2/kg2G = 6.674 \times 10^{-11}\ \text{N·m}^2/\text{kg}^2.

Gravitational Field Strength

g=GMr2g = \frac{GM}{r^2} At Earth's surface, g9.8 m/s2g \approx 9.8\ \text{m/s}^2.

Orbital Motion

For a satellite in circular orbit, gravity provides the centripetal force: GMmr2=mv2r\frac{GMm}{r^2} = \frac{mv^2}{r} vorbit=GMrv_{\text{orbit}} = \sqrt{\frac{GM}{r}}

Kepler's Third Law

T2r3T2=4π2GMr3T^2 \propto r^3 \quad \Rightarrow \quad T^2 = \frac{4\pi^2}{GM}r^3

Worked Example

Problem: A 1000 kg1000\ \text{kg} car travels around a flat circular track of radius 50 m50\ \text{m} at 15 m/s15\ \text{m/s}. What minimum coefficient of static friction is needed?

Solution:

The friction force provides centripetal force: fs=mv2r=1000(15)250=4500 Nf_s = \frac{mv^2}{r} = \frac{1000(15)^2}{50} = 4500\ \text{N}

Normal force on flat ground: FN=mg=1000(9.8)=9800 NF_N = mg = 1000(9.8) = 9800\ \text{N}.

μs=fsFN=450098000.46\mu_s = \frac{f_s}{F_N} = \frac{4500}{9800} \approx 0.46

Practice Questions

  1. 1. A ball on a 0.8 m0.8\ \text{m} string swings in a horizontal circle with period 0.5 s0.5\ \text{s}. What is the centripetal acceleration?

    v=2πr/T=2π(0.8)/0.5=10.05 m/sv = 2\pi r/T = 2\pi(0.8)/0.5 = 10.05\ \text{m/s}. ac=v2/r=101/0.8126 m/s2a_c = v^2/r = 101/0.8 \approx 126\ \text{m/s}^2.

    2. Calculate the gravitational force between Earth (5.97×1024 kg5.97 \times 10^{24}\ \text{kg}) and a 70 kg70\ \text{kg} person on the surface (r=6.37×106 mr = 6.37 \times 10^6\ \text{m}).

    F=GMm/r2=(6.674×1011)(5.97×1024)(70)/(6.37×106)2687 NF = GMm/r^2 = (6.674 \times 10^{-11})(5.97 \times 10^{24})(70)/(6.37 \times 10^6)^2 \approx 687\ \text{N}.

    3. A satellite orbits Earth at altitude h=400 kmh = 400\ \text{km} above the surface. What is its orbital speed? (Use RE=6.37×106 mR_E = 6.37 \times 10^6\ \text{m})

    r=RE+h=6.77×106 mr = R_E + h = 6.77 \times 10^6\ \text{m}. v=GM/r=(6.674×1011)(5.97×1024)/6.77×1067670 m/sv = \sqrt{GM/r} = \sqrt{(6.674 \times 10^{-11})(5.97 \times 10^{24})/6.77 \times 10^6} \approx 7670\ \text{m/s}.

    4. If the orbital radius doubles, by what factor does the orbital period change?

    T2r3Tr3/2T^2 \propto r^3 \Rightarrow T \propto r^{3/2}. Factor = 23/2=222.832^{3/2} = 2\sqrt{2} \approx 2.83.

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Summary

  • Centripetal acceleration is v2/rv^2/r, always directed toward the center.
  • Centripetal force is the net inward force — identify which real force(s) provide it.
  • Gravity follows an inverse-square law: F1/r2F \propto 1/r^2.
  • Orbital speed depends on the central mass and orbital radius, not the satellite's mass.

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