Learn / Gravity and orbits

What gravity is

The physics

The equations, worked through.

  1. First look
  2. How it works
  3. The physics
  4. The frontier, still to be written

The physics

The equations, worked through

This level puts numbers to the rules in the level before. Masses and sizes are from NASA’s fact sheets and JPL’s table of constants, and every result is worked out here and set beside a listed value where there is one.

Newton’s law. Two masses m1m_1 and m2m_2 whose centres are a distance rr apart pull on each other with a force

F=G m1m2r2F = \frac{G\, m_1 m_2}{r^2}

where G=6.67430×10−11G = 6.67430 \times 10^{-11} m³ kg⁻¹ s⁻². A sphere pulls on things outside it exactly as if all its mass were at its centre, which is why rr is measured between centres.

Why everything falls together. Newton’s second law says a force FF gives a mass mm an acceleration a=F/ma = F/m. For a mass mm falling towards a much larger mass MM,

a=Fm=GMr2a = \frac{F}{m} = \frac{G M}{r^2}

The falling mass has cancelled. A hammer and a feather get the same acceleration.

Surface gravity. At the surface of a body of radius RR the acceleration is

g=GMR2g = \frac{G M}{R^2}
Body GMGM (km³/s²) RR (km) Surface gravity (m/s²) Compared with Earth
Earth 398,600 6,371.0 9.82 1
Moon 4,902.8 1,737.4 1.62 0.165
Mars 42,828 3,389.5 3.73 0.380
Sun 132,712,000,000 695,700 274 27.9

The fact sheets list 9.820, 1.62, 3.73 and 274.0. The Earth’s spin and its slightly flattened shape bring what you feel at the equator down to 9.780.

At the height of the space station, 400 km up, rr is 6,771 km in place of 6,371, and the pull is weaker by (6371/6771)2=0.885(6371/6771)^2 = 0.885.

The balance point. Two bodies a distance dd apart go round their common centre of mass. Its distance from the centre of the first is

r1=d m2m1+m2r_1 = d\, \frac{m_2}{m_1 + m_2}

The Earth has 81.30 times the mass of the Moon, and the two are 384,400 km apart on average. That puts the balance point 384,400/82.30=4,671384{,}400 / 82.30 = 4{,}671 km from the Earth’s centre, about 1,700 km below the surface.

The Sun has 1,047 times the mass of Jupiter, which orbits at 778.479 million km. Their balance point is 742,600 km from the Sun’s centre. The Sun’s radius is 695,700 km, so the point lies 47,000 km above the visible surface.

Energy and escape. Lifting a mass mm against gravity stores energy. Counted from zero at a very great distance, the energy at distance rr is

U=−GMmrU = -\frac{G M m}{r}

To get away for good, a body needs enough energy of motion to bring the total up to zero: 12mv2=GMm/R\tfrac{1}{2} m v^2 = GMm/R. The mass cancels again, and

vesc=2GMRv_{\text{esc}} = \sqrt{\frac{2 G M}{R}}

This gives 11.19 km/s for the Earth and 617.7 km/s for the Sun. The fact sheets list 11.186 and 617.6.

Where Newton runs out. General relativity agrees with Newton’s law whenever gravity is weak and speeds are small. A useful measure of how weak is the number GM/(rc2)GM/(rc^2), with cc the speed of light. At the surface of the Earth it is 7×10−107 \times 10^{-10}. At the surface of the Sun it is 2×10−62 \times 10^{-6}. Einstein’s corrections are of this size, which is why they went unnoticed for so long. Three of them have simple formulas.

Light passing a mass. A ray that passes a mass MM at closest distance bb is bent through an angle

α=4GMc2 b\alpha = \frac{4 G M}{c^2\, b}

For light grazing the edge of the Sun this is 8.49×10−68.49 \times 10^{-6} radians, or 1.75 seconds of arc. The measurements of 1919 were good to only about 30 per cent. Radio telescopes have since confirmed the figure to 0.02 per cent.

Mercury’s orbit. On each orbit the nearest point to the Sun moves forward by

Δϕ=6πGMc2 a (1−e2)\Delta\phi = \frac{6\pi G M}{c^2\, a\,(1 - e^2)}

For Mercury, a=57.909a = 57.909 million km and e=0.2056e = 0.2056, which gives 0.1035 seconds of arc for each orbit. Mercury goes round 415 times in a century, so the total is 43.0 seconds of arc a century. The amount left unexplained by Newton’s law was 43.

Clocks. A clock at distance rr from a mass runs slow, compared with one far away, by the fraction GM/(rc2)GM/(rc^2). A clock moving at speed vv runs slow by v2/(2c2)v^2/(2c^2). For the clocks on navigation satellites the first effect is a gain of 46 microseconds a day over clocks on the ground, because they are higher up, and the second is a loss of 7, because they are moving fast. The net gain is 39 microseconds a day. Light travels 11.7 km in that time, so a system that ignored the difference would drift by that much each day.

Where this comes from

The words are written for this site. Sums in the text are worked from the figures in these sources.