At some time, this is the combined picture of what the observers from point A and B see. Line p represents the parallax of Venus, which corresponds to angle B’VA’ in Fig. 6.
Another variable we need to measure is the distance AB, which could be found by knowing the latitude φ, longitude λ and Earth’s radius:
“l” you get is the length AB.
Kepler’s third law states that the cube of a planet’s distance from the Sun is proportional to the square of its orbital period. The orbital period of Earth is 1 year while the orbital period of Venus is 0.62 year. From these information, we have:
That means we have the ratio of the distance from Earth to Sun (ES) and the distance from Venus to Sun (VS).
Fig. 8 Points E, V, B’, A’, and S
Figure 9
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