Roemer observed a difference in the length of time during which a certain moon of Jupiter was occulted by the planet’s body, and found that this difference underwent regular changes coincident with the changes in the earth’s position in relation to Jupiter and the sun. Seen from the sun, the earth is once a year in conjunction with Jupiter, once in opposition to it. It seemed obvious to explain the time-lag in the moon’s reappearance, when the earth was on the far side of the sun, by the time the light from the moon needed to cover the distance marked by the two extreme positions of the earth – that is, a distance equal to the diameter of the earth’s orbit. On dividing the observed interval of time by the accepted value of this distance, Roemer obtained for the velocity of light a figure not far from the one found later by terrestrial measurements.