brief history of the Sun which we
included in these pages gives you a comprehensive and perhaps
complicated introduction to the Sun as a star in our galaxy, the Milky
Way. Stars are very different objects than are planets. They are very
large and are giving off immense amounts of radiation.
This activity requires a sunny day and a cheerful disposition towards math!
Be sure to remind students that looking at the Sun can cause
permanent eye damage -- never look at the Sun directly!
Materials: 8 1/2 x 11 inch sheets of paper, yard(meter)sticks, tape, pencils, index
cards, straight pin
As we pointed out on the Sun history page, most of the
stuff in the Solar System is in the Sun, leaving very little
for the planets, moons, and us! It is difficult
to imagine how large a star is without seeing it up close; however, we can do a
quick experiment to calculate the size of the
closest star to us, our Sun.
ACTIVITY: How big is the Sun?
Now some quick relations involving space and math! Ask students if they have ever made scale models of planes, boats, people...How does scale modeling work? Students should understand the idea of ratios, factors of difference between two sizes. In the case of the Sun, we know that the the distance between the two lines, or the size of the little light spot, was recorded by the students in the first step and should be around 2mm. We also know that the students recorded how far away from the source of the light (the prick hole) the spot is by the number they recorded for the distance they needed to place the paper from the prick hole to make the spot fill the lines. So, they should then have a 2mm spot which is around 218mm away from the source hole. If we wanted to move the paper further away, could we guess by how much the spot would grow? What if the paper were over 93 million miles away?!
The ratio between the distance to the spot and the width of the spot is the value of the recorded distance divided by the recorded spot size. Students should use their own recorded values, but for this explanation, we will use the ones we guessed above.
Distance to the spot is 218mm. Size of the spot is 2mm. So, 218 divided by 2mm is 109.
The number 109 is the ratio of the two measurements and will be our guide in determining
the size of the Sun. Since we are using the sunlight as a guide, and we have found a direct
relationship (ratio) between the distance of the light and the size of the light spot, we can
make direct conclusions about the Sun itself. (Similarly, if we were using a flashlight, we
could make determinations about it). If the distance of the Sun is around 93 million miles,
then the size of the Sun will be found like so: Distance to Sun is 93 million miles
(93,750,000 to be exact). Size of the Sun is unknown, but the ratio from the observations
is 109. So, 93,750,000 miles divided by size of the Sun is 109. Another way to say that is
93,750,000 miles divided by 109 is the size of the Sun. Ha ha! So...
Is the size of the Sun surprising when students consider the size of the Earth is 8,000 miles across? Is the Sun really anything similar to the Earth? Was the ratio relation easy to understand and use? Did students find the math difficult or powerful? How could students use the ratio relation to measure other things? What about the size of the Moon? Try holding a pencil out at arm's length towards the full moon. The pencil width should just wink out all of the moon's face. If you know the width of the pencil and the distance between it and your eyes, now you can find the ratio! Divide the distance to the moon (250,000 miles) by this ratio, and you have found the size of the moon!
If you ask students what a particular season means to them, they'll probably mention the weather usually associated with it. Summer is hot. Winter is cold. Spring and Fall are in between. (For those of us living close enough to the poles, winter means snow, too!) A common misconception (even among a disturbingly large number of college graduates) is that the Earth is closer to the Sun during the summer, causing summer's warmer temperatures. This model, of course, is inconsistent with the fact that while the Northern Hemisphere has summer, the Southern Hemisphere has winter. Furthermore, while it is summer for the Northern Hemisphere, the Earth is actually slightly farther away from the Sun than during the Northern Hemisphere winter.
During the Northern Hemisphere's summer, the North Pole is tilted towards the Sun. During the winter, it is tilted away. This tilt causes the Sun to appear higher in the sky during the summer than during the winter. The higher Sun causes more hours of daylight and more intense, direct sunlight, or hotter conditions on the surface of the Earth. Questions to ask the class include: How is summer different from winter? What changes as winter gives way to spring? What changes are there as summer becomes fall? What about when winter approaches?
It is important to note that even without the tilt of the Earth, there would still be
variations in temperature from one location to another, caused mainly by the curvature of
the earth. Locations closer to the equator would still, on the average, be warmer than
locations closer to the poles. Light and heat (radiation) from the Sun would still strike
polar regions at more of an angle than nearer the Equator. This angle tends to "spread out"
the same amount of energy over a larger area, thereby decreasing its intensity and the
amount of heat it brings to the Earth. The activities addressing this topic demonstrate and
test this assertion.
Be sure to remind students that looking at the Sun can cause permanent eye damage -- never look at the Sun directly!
Solar radiation is emitted in various forms which travel at the speed of light. Light travels through space as waves of different lengths. Our eyes can only see radiation as visible light, but radiation also occurs as radio waves, infrared rays, ultraviolet rays, X- rays and gamma rays. Together these waves make up the electromagnetic spectrum. The sunlight reaches the Earth mostly as visible, infrared, and radio light; the upper atmosphere blocks most of the other wavelengths. When the light reaches the ground it is absorbed into the grass, rocks, people, soil, etc. and becomes heat energy. How else could we "feel" sunlight if it did not have the ability to change into heat?
Questions to ask: How much energy is the sunlight creating on the Earth? How can we
measure the warmth from the Sun? What might influence fluctuations in warmth? What
experiences have students had which help in these predications? Will soil be warmer or
colder than air temperature? Does this change during the day? During the year?
Materials: thermometers; soil; sunlight; index cards; stick; pencils
Students discuss results of these experiments. What caused the highest or hottest
temperature? Was this related to the time of day? What were students able to discover from
their measurements? How accurate were their predictions? What factors helped them to
predict well? What conclusions can they make about the effect of the Sun's rays on the
Earth? If done at intervals over a period of time, did earlier experiments help their
predictions? What would happen if the experiment were done in a couple of months?
ACTIVITY: How Angle Spreads Sunlight
Be sure to remind students that looking at the Sun can cause permanent eye damage -- never look at the Sun directly!
The previous activity allowed students to observe the energy of the sunlight. However,
since the angle of the sunlight influences the amount of energy it creates, it is important for
students to observe this effect to understand why the winter on the Earth is colder than the
summer is. This activity shows how light falling upon a tilted surface is less intense than if
it were falling directly, demonstrating this "spreading out" of light by measuring how
quickly and by how much the sunlight can warm two sheets of paper: one tilted, one not.
Materials: Two sheets of black construction paper; two pieces of cardboard or
plywood; bricks or blocks to prop up board; masking tape; two
thermometers.
the board and the paper, and the scale can be read without
removing the thermometer. Tape the thermometers in place.
Leave the assembled thermometers (we'll call them
"contraptions"!) in the shade long enough so that they read the
same outside temperature.
Which paper's temperature rose more quickly? What was the angle of the Sun when the
temperature was the highest for each thermometer? Can the students make a relation
between the angle of the sunlight and the affect on the Earth from seeing the affect on the
tilted paper? How high is the Sun at noon in the summer versus how high the Sun is at noon
in the winter? Try to make a connection between the tilt of the Earth in the summertime and
the summer temperatures as well as the tilt of the Earth in the wintertime and the winter
temperatures. What if the Earth was not tilted? Would there be any seasons?
Introduction to Astronomy in Motion Sun pages