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D · 5 · D.1 · Orbital motion, escape speed

Orbits and escape speed

Gravity as the centripetal force: orbital speed, period, the energy of a satellite, and how fast to leave for good.

HLHarder28 minFree
Hook

The International Space Station moves at 7.7 km every second and never hits the ground. Is it escaping gravity, or falling?

Orbital motion
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Gravity is the centripetal force

WORKED EXAMPLE · ORBITAL SPEED OF A SATELLITE

A satellite of mass m moves at constant speed v in a circle of radius r (measured from the centre) around a planet of mass M.

    “The acceleration of an object in circular motion is a = v² / r, directed to the centre. Here it equals g = GM / r², the field strength at that radius.”

    Check 1 of 7

    A satellite moves in a circular orbit of radius r around a planet of mass M. Its orbital speed is…

    Check 2 of 7

    A satellite is moved from an orbit of radius r to an orbit of radius 4r around the same planet. Its orbital speed becomes…

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    Satellite A orbits a planet at radius r with period T. Satellite B orbits the same planet at radius 4r. The period of B is…

    Check 4 of 7

    A satellite of mass m moves in a circular orbit of radius r around a planet of mass M. Its total energy is…

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    The escape speed from the surface of a planet of mass M and radius R is…

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    A 500 kg research satellite is in low Earth orbit at radius 6.78 × 10⁶ m. Its kinetic energy is about…

    Check 7 of 7

    The escape speed from a moon is 12 km s⁻¹. A probe moves in a circular orbit just above its surface. Its orbital speed is about…

    Apply

    An astronaut on the ISS says: “There is no gravity up here, that is why I float.” Use the ideas of this lesson to explain what is wrong.

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    Remember earlier lessons
    From lesson D · 4

    Gravitational potential V_g = −GM / r is…

    From lesson D · 2

    The distance to a mass is doubled. The field strength g becomes…

    Summary card

    Key points

    • • Gravity provides the centripetal force: v = √(GM / r), independent of the satellite’s mass.
    • • T² = 4π² r³ / (GM), so r³ ∝ T² (Kepler’s third law).
    • • KE = GMm / 2r, GPE = −GMm / r, TE = −GMm / 2r = −KE.
    • • Escape speed v = √(2GM / R) makes the total energy zero. It is √2 times the orbital speed at that radius.

    Formulas

    • v = √(GM / r)
    • T² = 4π² r³ / (GM)
    • TE = −GMm / 2r
    • vesc = √(2GM / R)

    Key terms

    Orbital radius
    :
    distance from the centre of the planet to the satellite
    Escape speed
    :
    the minimum launch speed to reach infinity with no more propulsion
    Free fall
    :
    motion under gravity alone, which feels weightless

    Common errors

    • • Using the height above the surface as the orbital radius.
    • • Thinking a faster satellite must be in a higher orbit.
    • • Giving a bound satellite a positive total energy.
    Checks solved: 0 of 7