Part I: The Reasons for the Seasons
Below are three facts about the seasons that we wish to explain. Below the facts are four hypotheses about what might cause the seasons to occur. Your job is to think about each one and figure out which of the four hypotheses are most right and which ones are wrong. Be sure to keep these three facts in mind while going through the lab.
Key facts about the seasons:
I. In northern latitudes, it’s warm in June/July and cool in Dec/Jan, on average.
II. In southern latitudes, the seasons are reversed: it’s warm in Dec/Jan and cool in June/July.
III. It’s warmer at latitudes close to the equator than at latitudes close to the poles (on average).
Hypothesis #1: The Sun-Earth distance changing due to
Earth’s elliptical orbit causes the seasons.
If its orbit were a circle, the Earth would always be the same distance from the Sun. But it’s not. The orbit is an ellipse. As compared to the average Earth/Sun distance, the Earth is sometimes 1.7% closer and at other times 1.7% farther away from the Sun than the average.
Is this difference significant? To answer this question, it helps to be able to refer to a scale model of the Sun/Earth system. Recall the scale model of the solar system we made in Lab 1. We made the size of the Sun and Earth and the distance between them all smaller by the same factor: 1010. Let’s repeat these calculations for the Earth-Sun system.
Sun diameter: 1.4 × 106 km → scale model Sun diameter = 14 cm
To get the above, remember that we divide by the scale factor to shrink the normal size:
1.4 × 106 km 1010
= 1.4 × 10−4 km
Then we convert to units of cm:
1.4 × 10−4��km × 103m
1��km = 1.4 × 10−1��m ×
1��m = 1.4 × 101cm = 14cm
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Now try to get the values for the Earth diameter and the Earth-Sun distance, you can also look up the values from Lab 1, but make sure they are right:
Earth diameter: 1.3 × 104 km → scale model Earth diameter = cm
→ scale model Earth diameter = mm
Earth-Sun distance: 1.5 × 108 km → scale model distance = m
A 1.7% change in the Earth-Sun distance is thus:
scale model Earth-Sun distance = m ×0.017 = m = cm
To make sure we all have the same model, you may remember, the Sun was represented by a small watermelon, the Earth would be about the size of a candy sprinkle and the distance between them would be the size of an apartment, small house or a big great room inside a medium/large house (15 meters).
Now that we have the Earth-Sun model in our heads, imagine standing in one corner of a big room holding the tiny Earth sprinkle and you see the watermelon Sun in the other corner of the room. Also pretend that the watermelon is sitting in a bon fire, this will represent the heat we feel from the Sun.
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Hypothesis #2: The change in the Sun-Earth distance due to
the tilt of the Earth causes the seasons.
In the summer months, the northern hemisphere of Earth tilts 23.5 degrees toward the Sun, while in the winter months, it tilts away from the Sun. Another hypothesis we could make is that the hemisphere that is tilted toward the sun is warmer because it’s closer to the Sun than the hemisphere that is tilted away from the Sun. (See diagram from Prather, Slater, Adams, and Brissenden below)
To test this hypothesis, consider the scale model you constructed. Try tilting the North Pole of your model Earth toward or away from the model Sun on the other side of the room (without changing the distance from the center of the Earth to the Sun).
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Hypothesis #3: The change in the length of the day due to the
tilt of the Earth’s axis causes the seasons.
Before going into how the length of the day changes due to the tilt, let’s focus on the tilt itself. The image below shows how over the course of a year (orbit) the tilt stays the same. Why is that? Recall that the Earth’s spin axis points at the North Celestial Pole, a point on the Celestial Sphere that is very close to Polaris, also known as the North Star. It keeps pointing steadily at the same position as the Earth goes around the Sun. (Recall that precession occurs so slowly that even over your whole lifetime, the effect will be very small and can be ignored for most purposes.)
Figure 1: source: https://www.timeanddate.com/astronomy/equinox-not-equal.html
Notice how when it is the Summer in the Northern hemisphere and Winter in the Southern Hemisphere (June), the North Pole is tilted towards the Sun while the South Pole is tilted away. Also notice that when it is the Winter in the Northern Hemisphere and Summer in the Southern Hemisphere (December), the North Pole is tilted away from the Sun and the South Pole is tilted towards the Sun. The two Earth’s in the middle of the diagram are neither tilted towards or away from the Sun. This is when it is Spring and Autumn in the Northern and Southern Hemispheres.
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Now let’s see what effect the tilt has on the length of days. Watch the youtube video linked below and answer the following questions. Remember, you can always pause and rewind the video if you missed something! (Note: If you are in a place that can’t access YouTube, you can still answer the questions below by using Figure 1 above.)
Video break down:
a. Does it look like the North Pole gets both day and night? If not, what does it get?
b. What is happening in Antarctica (South Pole)? Does it get day and night? If not, what does it get?
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a. Has anything changed about the amount of daylight at the North or South Poles? If so, describe the changes.
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Hypothesis #4: The change in the intensity of the Sun’s rays
due to the tilt of the Earth’s axis causes the seasons.
The changing tilt of Earth relative to the Sun also affects the intensity of the Sun’s rays on different parts of the Earth at different times of the year. First, let’s compare the intensity of the Sun’s rays in the summer vs. winter in northern latitudes on Earth.
Figure 2: source: https://media.nationalgeographic.org/assets/photos/000/312/31279.jpg
Pay attention to Earth A on the left. Notice how the North Pole is tilted towards the Sun, also notice how the most direct Sun rays (shown in brighter yellow) land above the Earth’s equator in the Northern Hemisphere and how the Sun’s rays seem to just graze the Southern Hemisphere.
Now pay attention to Earth B on the right. The North Pole is now pointing away from the Sun. Notice now how the Sun’s most direct rays fall below the Earth’s equator in the Southern Hemisphere and that they only graze the Northern Hemisphere.
a) Earth A?
b) Earth B?
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The image below shows how these direct sun rays land on the Earth during the Summer and how the indirect rays land on the Earth during the Winter. Notice how the same amount of rays land on the Earth in both Summer and Winter, but during the Summer the rays land in a smaller area then in the Winter.
Figure 3: source: https://physics.weber.edu/schroeder/ua/SunAndSeasons.html
You can test this for yourself by using a flashlight (or phone flash light). Point the light directly at a table (perpendicular) to represent Summer, then point the light at an angle (45◦) to represent Winter. You can also test this by using a small space heater. If you point the heater directly at yourself you may notice how much hotter it feels than if it were pointed next to you.
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For Fun: Here is a short Bill Nye video explaining the seasons: https://youtu.be/ KUU7IyfR34o
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Part II: The Sun, Solstices, Equinoxes, and Seasons on Earth
Apparent motion of the Sun (Hint: refer to Lab 7 if you are having trouble remembering)
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The Solstices and Equinoxes
Since the Earth is tilted relative to the plane defined by the Earth’s orbit around the Sun, the apparent path of the Sun is not along the Celestial Equator, but instead follows a path in the sky known as the “ecliptic”. The ecliptic is tilted by 23.5 degrees relative to the Celestial Equator.
Over the course of one year, the Sun completes one cycle around the ecliptic. On the following four dates, the Sun is at the following special locations:
Mar. 21: the Vernal Equinox the first day of spring (the Sun crosses the Celestial Equator, moving north)
June 21: the Summer Solstice the first day of summer (the Sun is as far north on the Celestial Sphere as it gets)
Sept. 21: the Autumnal Equinox the first day of autumn (the Sun crosses the Celestial Equator, moving south)
Dec. 21: the Winter Solstice the first day of winter (the Sun is as far south on the Celestial Sphere as it gets)
In this exercise we will use Stellarium to explore three of the effects of the Earth’s tilt by checking how the Sun’s behavior compares on these various dates. These behaviors are related to the seasons. In particular, we will measure: (1) the length of the day; (2) the compass positions where the Sun rises and sets; and (3) the altitude of the Sun at noon.
1) Set the location. We are all going to use San Francisco as our location so that we can all see the same constellations. At the bottom of the webpage you should see a button that tells you where you’re observing from. It’ll say “near (location),” click that button. Once the map pops up, drag the location pin to San Francisco and click “> use this location” above the map. Also make sure that the toggle for “Use Autolocation” is turned off.
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2) Turn on/off icon features. At the bottom, you’ll also see a bunch of symbols which will turn on and off certain features of the night sky. Turn on the “Constellations” and turn off the “Atmosphere” symbol as shown below. If this isn’t done, you won’t be able to see the stars!
3) Turn on the Meridian. Click the three horizontal line icon in the top left of the screen and look for “View Settings”. Open the settings and check the box that says “Meridian Line”. Once done, you can close out of the settings menu. If you look around the sky, you should notice that the Meridian is a line in the sky (much like the Prime Meridian on Earth) that goes from due North on the horizon through your Zenith (90àaltitude) to due South again on the horizon. It essentially divides the sky into an Eastern and Western halves.
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