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There are two points in time every year when the Sun s elevation, measured with respect to the center of its disk, is positive for exactly 12 hours and negative for exactly 12 hours One of these time points occurs on March 21,
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Figure 3-1 Azimuth based on a southerly point of reference
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give or take about a day; the other occurs on September 22, give or take about a day At the equinoxes, the Sun is exactly at the celestial equator; it rises exactly in the east and sets exactly in the west, assuming that the observer is not at either of the geographic poles The names vernal and autumnal, as used in the northern hemisphere, are not really correct in the southern hemisphere because the seasons are reversed compared with those in the north Thus it is best to speak of the March equinox and the September equinox The crude celestial maps of Fig 3-2 show the situation at either equinox That is, the date is on or around March 21 or September 22 You can deduce this because the Sun rises exactly in the east and sets exactly in the west, so it must be at the celestial equator At the latitude of Sydney, the Sun is 35 degrees away from the zenith (55 degrees above the northern horizon) at high noon on either of these days The south celestial pole, which unfortunately has no well-defined sentinel star, as is the case for the northern hemisphere, is 35 degrees above the southern horizon all the time The heavens seem to rotate clockwise around the south celestial pole In the drawing at A, imagine yourself lying flat on your back, with your head fac-
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PART 1
The Sky
Sun East 60 30 0 West
South South
West 60 Sun 30 0
East
North Figure 3-2 Az/el sky maps for midafternoon at 35 degrees south latitude on or around the March
or September equinoxes At A, top of head facing north; at B, top of head facing south
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ing north and your feet facing south In the drawing at B, imagine yourself rotated 180 degrees, that is, with your head facing south and your feet facing north Either orientation is valid astronomically, and you will find star maps that use either scheme Every day the Sun moves slightly toward the east with respect to the background of stars At the March equinox, the Sun is at the celestial equator and is located in a certain position with respect to the stars This represents the reference point for right ascension (RA) and declination (dec) As time passes, the Sun rises about 4 minutes later each day relative to the background of stars The sidereal (star-based) day is about 23 hours and 56 minutes long; the synodic (sun-based) day is precisely 24 hours long In the southern hemisphere, the Sun s motion relative to the stars is from left to right In the drawings of Fig 3-2, the Sun is at dec = 0 degrees Suppose that these drawings represent the situation at the March equinox This point among the stars is the zero point for right ascension (RA = 0 h) As autumn passes and the Sun follows a lower and lower course across the sky, the declination and right ascension both increase for a while Remember that right ascension is measured in hours, not in degrees There are 24 hours of h right ascension in a circle, so 1 hour (written 1 h or 1 ) of RA is equal to 15 degrees
THE SUN S ANNUAL LAP IN THE SOUTH
Let us begin following the Sun during the course of the year starting at the March equinox As the days pass during the months of April, May, and June, the Sun stays above the horizon for less and less of each day, and it follows a progressively lower course across the sky The change is rapid in the first days after the equinox, and becomes more gradual with the approach of the June solstice, which takes place on around June 22 give or take a day This might be called the winter solstice, but again, to avoid confusion with northern-hemisphere-based observers who call it the summer solstice, it is better to name the month in which it occurs At the June solstice, the Sun has reached its northernmost declination point, approximately dec = +235 degrees The Sun has made one-quarter of a complete circuit around its annual lap among the stars and sits at RA = 6 h This situation is shown in Fig 3-3 using the same two az/el coordinate schemes as those in Fig 3-2 The gray line represents the Sun s course across the sky As in Fig 3-2, the time of day is midafternoon The observer s geographic latitude is the same too: 35 S
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