Its winter in the Northern Hemisphere and were at our closest point to the Sun. Closest? Yes, you read that right. Closest. For northerners, the winter solstice has just passed. But the truth is, on January 3, 2007, Earth reaches perihelion, its closest point to the Sun in its yearly orbit around our star. At first glance, it makes no sense. If Earth is closest to the Sun in January, shouldnt it be summer? Maybe, if you live in the Southern Hemisphere. So what does this mean? Earths orbit is not a perfect circle. It is elliptical, or slightly oval-shaped. This means there is one point in the orbit where Earth is closest to the Sun, and another where Earth is farthest from the Sun. The closest point occurs in early January, and the far point happens in early July (July 7, 2007). If this is the mechanism that causes seasons, it makes some sense for the Southern Hemisphere. But, as an explanation for the Northern Hemisphere, it fails miserably. In fact, Earths elliptical orbit has nothing to do with seasons. The reason for seasons was explained in last months column, and it has to do with the tilt of Earths axis. But our non-circular orbit does have an observable effect. It produces, in concert with our tilted axis, the analemma. If you plot the noontime position of the Sun in the sky over a one-year period, it produces a figure-eight shape on the sky. This is the analemma. You may have seen it drawn on a globe of Earth. The shape results from the combination of two things: the 23.5° tilt of Earth on its spin axis, and the elliptical shape of Earths orbit around the Sun. The highest point on the analemma is the Suns noon position on the summer solstice. The lowest point marks the winter solstice. The difference in the Suns noontime height in the sky is caused by Earths tilted axis. What about the left-to-right variation in the analemmas curve? Thats where our elliptical orbit comes in! Notice the vertical line running up from the south point on the horizon? Thats the meridian. The meridian runs straight up and over the sky, from due north to due south. If Earths orbit was a perfect circle, the Sun would cross the meridian at noon every day (ignoring daylight savings time). But our orbit is slightly oval-shaped. In July, we are at our furthest point from the Sun, and Earth moves slower than average along its path. In January, we are closer to the Sun, and Earth speeds up a bit in its orbital progress. The result of this change in speed means the Sun crosses the meridian a little early, or a little late, depending on where Earth is in its orbit. For all points along the curve to the left of the meridian, the Sun is slow. It crosses the meridian after 12:00 p.m. For all points along the curve to the right of the meridian, the sun is fast, crossing the meridian slightly before noon. Astronomers call this the equation of time. It is marked on many sundials. The equation of time is defined as the difference between true solar time (determined by the Suns position in the sky) and mean solar time (the time told by your watch). The two times can vary by as much as 16 minutes over the course of a year. Earth reaches perihelion on January 3, 2007 (Figure C). The Earth-Sun distance will be 147,093,602 km. Aphelion, the greatest distance from the Sun, occurs on July 7, 2007, when the Earth-Sun distance will be 152,097,053 km. The difference between the two is 5,003,451 km, (3.3 percent), and not enough to cause the seasons. Even though, at this time of year, were as close to the Sun as we can get, for the Northern Hemisphere, it will always be winter.
Posted on: Mon, 05 Jan 2015 21:03:57 +0000