In an age when the size of the observable universe is known to a few decimal places, today’s Transit of Venus offers a good opportunity to reflect on just how far we’ve come.
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Less than 250 years ago, the brightest minds of the Enlightenment were stumped over how far the Earth is from the sun. The transits of the 1760s helped answer that question, providing a virtual yardstick for the universe.
Without an accurate distance between the sun and Earth — known as the Astronomical Unit — astronomers couldn’t deduce the exact size of the solar system and had no way of knowing for sure how far away the stars were.
The Astronomical Unit has been “fundamental to figuring out the distances of everything in astronomy,” says Michael Strauss, a professor of astrophysics at Princeton University.
Enter Edmond Halley of comet fame. In 1716, he alerted the scientific community to be ready for the 1761 and 1769 transits of Venus. He noted that if Venus were observed from multiple spots as it crossed the disc of the sun, you could use something called the parallax method and some trigonometry to get the much sought-after sun-Earth distance.
Although Halley, who died in 1742, was long gone by the transits of the 1760s, his historical timing was nonetheless impeccable. “This was the Age of Discovery, and people were finally able to start mounting big expeditions around the world for all kinds of reasons,” Strauss says.
So an international effort was organized, with nations dispatching expeditions to far-flung places. Legendary English navigator and explorer Captain James Cook was among them. He and his team sailed aboard the HMS Endeavour to newly discovered Tahiti in the South Pacific, where observations were set up ahead of the 1769 transit. (Observations in 1761 were largely failures.)
So, how did the parallax method work?
“You observe the moment at which Venus touches the disc of the Sun, what’s called first contact,” Strauss says. “What you’re measuring is when Venus, the Sun and the observer all appear to be in a straight line.”
From different locations on Earth, that lining up occurs at slightly different times. It takes about seven hours for the total transit, so the difference between observations might be as much as a few minutes – easily measured by clocks of the day.
“You want to know exactly how long it takes, because that duration gives you a [base] line and that line you can then fit onto the sun,” says Owen Gingerich, a professor emeritus of astronomy and the history of science at Harvard University.
The line forms the base of a right triangle, and right triangles make good yardsticks, says Gingerich, who spoke to NPR from California, where he is preparing to observe today’s transit.
By knowing the exact distance between the two Earth-bound observers and comparing the differences in their observations, you can draw a pair of triangles that will give the distance from the Earth to Venus. Thanks to the work of mathematician Johannes Kepler, 18th century astronomers already knew Venus’ orbit is about 70 percent that of Earth’s. So if you know the distance between the Earth and Venus, you can easily figure out the value for the Astronomical Unit.
But it wasn’t that simple. Because of something called the “black drop effect” having to do with density differences in the sun’s outer layers, the observations were a little skewed. That threw the post-1769 figure for the Astronomical Unit off by a few percent from the correct answer. Still not bad, actually.
And how did the transit of Venus give us the distances to the stars?
The parallax method turns out to be good for figuring out how far they are, too. But since the stars are so much more distant than Venus, a much longer baseline was needed. Instead of two different geographic locations, the observations needed to be made during two different points in Earth’s orbit, say one in June and another in December. Knowing the length of the Astronomical Unit (and therefore the size of the Earth’s orbit) allowed scientists to know just how long the base of that massive right triangle would be.