Skygazing/Solar eclipse lab on a sunny day
PurposeEdit
To measure the size of the Moon's penumbra during a solar eclipse using a scale model.
Why this is a scale modelEdit
A scale model is a drawing that preserves all the angles. Here we represent the Moon as a small Styrofoam ball. The Earth is most easily represented as a map of a region where a solar eclipse is expected. Here we use the United States.
For the Sun, we use the actual object, which of course is not to the same scale. But for our purposes, any object that produces light with the proper angular distribution can be used. In other words, the actual Sun provides the required angular spread of light rays (i.e., light spread over a range of about half a degree). The actual size of the Sun is irrelevant (otherwise one could use a solar eclipse to calculate the size and distance to the Sun).
EquipmentEdit
 10 ft rod to hold up the model "Moon" (we clamped a twometer stick to a onemeter stick)
 One inch diameter ball to server as the Moon (rod and ball dimensions may vary proportionally)
 Tape measure or other way to measure distance on the ground (we used 2 metersticks)
 Camera (we used an Apple iPhone)
 White screen. We used about a dozen sheets of paper. It would also be worthwhile to print onto this paper a properly scaled image of a region on Earth, or perhaps the Earth itself.
 At least two people (three works better)
 The Sun on a sunny day
 The instructor and students should be mentally prepared to do calculations and proportional reasoning on three different scales:
 The solar system (especially Earth/Moon system)
 A scale where the Moon is reduced to a small ball
 A scale on which photos of the shadow are analyzed
ProcedureEdit
 The Moon was a one inch diameter styrofoam ball attached to a stick that was 110 inches long (chosen to match the EarthMoon distance).
 We forgot to measure the altitude of the Sun. Fortunately the images on commons contain a time stamp and we know where we were (Celina, Ohio). Somewhere a website will give us that angle.
 Photograph the shadow alongside a ruler for scale.
 Record the location of the shadow so that you may later calculate the distance from the "Moon" at the end of the stick and the "Earth", represented by the white paper on the ground.
How far from the model "Earth" should we hold the model "Moon"?Edit
 The Moon is about 60 earthradii from Earth.
 The Moon has a diameter about 1/4 that of the Earth.
 Our Styrofoam "Moon" had a diameter of one inch.
Keeping track of scaled objects can be confusing. One trick is to use capital letters for the real thing and lower case for the scale:
 equals scaled distance from Earth to Moon
 is the actual distance.
 equals scaled radius of Earth
 is the actual radius.
 equals scaled radius of the Moon
 is the actual radius.
Focusing on only astronomical data, we have:
Since we conclude that the Styrofoam ball should be held at a distance of
away from the Earth. Our "model" Earth was just a piece of paper, but we can add a scale to it using the fact that a one inch diameter ball represents the 2159 mile diameter Moon.
Calculating the scaleEdit
The scale is:
where we have used the "hat" notation to define the "scaled" inch. This "scaled" inch equals 2159 miles, but is also one (actual) inch on the scale model.
In other words, our scale is 1.37 x 10^{8} to 1.
Scaling the USAEdit
http://www.distance.to/NewYork/SanFrancisco says that the distance between NYC and SF is 2566 miles = 1430 km. Convert this to centimeters and divide by the scaling factor to get:
This says that the penumbra is larger than the USA? This seems to big, but see below. This experiment should be repeated and the results reported here.
Other photos from the experienceEdit
Understanding the size of the penumbraEdit
This diagram explains why the penumbra of a solar eclipse is approximately twice the size of the Moon. Since the Sun and Moon have nearly the same angular diameter, the umbra is reduced to nearly a single point in length. Therefore the three angles marked in red are nearly equal, all with a base equal to the Moon's diameter.
ConclusionEdit
If you go here http://eclipse.gsfc.nasa.gov/SEgoogle/SEgoogle2001/SE2017Aug21Tgoogle.html, you will see that the penumbra is very large and extends far outside the USA. Perhaps our results are correct.
We measured the length of the shadow on the photograph marked 0cm. It was projected on a classroom screen at a scale where 4.9 cm* equals 1 cm. In other words, the classroom projected image of the photo expanded the meter stick so that 1 cm on the stick measured 4.9cm* on the screen.^{[6]}. The shadow's length on the screen was 21 plus/minus 1 cm*. We concluded that the umbra was
1.69 ± 0.08 inches^{[7]}
This much smaller than the 2 inch umbra we expected from a 1 inch moon. Perhaps the brightest part of the penumbra was indistinguishable from the illuminated portion of the paper.^{[8]}
Test the hypothesis:How big is the umbra in this nasa gif?Edit
It looks to me that the height of the umbra is approximately equal to the radius of the Earth. According to https://nssdc.gsfc.nasa.gov/planetary/factsheet/moonfact.html, the ratio of diameters for the Earth to the Moon is:
Let be the diameter of the umbra, which we estimate to be equal to the radius of Earth and also twice the diameter of the Moon, but since the diameter of the Moon is twice its radius, we have:
Not bad!
W:On the Sizes and Distances (Aristarchus)Edit
The article on Wikipedia is excellent:
copied from w:Special:Permalink/773165157


Half Moon Aristarchus began with the premise that, during a half moon, the moon forms a right triangle with the Sun and Earth. By observing the angle between the Sun and Moon, φ, the ratio of the distances to the Sun and Moon could be deduced using a form of trigonometry. From the diagram and trigonometry, we can calculate that The diagram is greatly exaggerated, because in reality, S = 390 L, and φ is extremely close to 90°. Aristarchus determined φ to be a thirtieth of a quadrant (in modern terms, 3°) less than a right angle: in current terminology, 87°. Trigonometric functions had not yet been invented, but using geometrical analysis in the style of Euclid, Aristarchus determined that In other words, the distance to the Sun was somewhere between 18 and 20 times greater than the distance to the Moon. This value (or values close to it) was accepted by astronomers for the next two thousand years, until the invention of the telescope permitted a more precise estimate of solar parallax. Aristarchus also reasoned that as the angular size of the Sun and the Moon were the same, but the distance to the Sun was between 18 and 20 times further than the Moon, the Sun must therefore be 1820 times larger.
Aristarchus then used another construction based on a lunar eclipse: By similarity of the triangles, and Dividing these two equations and using the observation that the apparent sizes of the Sun and Moon are the same, , yields The rightmost equation can either be solved for ℓ/t or s/t The appearance of these equations can be simplified using n = d/ℓ and x = s/ℓ. The above equations give the radii of the Moon and Sun entirely in terms of observable quantities. The following formulae give the distances to the Sun and Moon in terrestrial units: where θ is the apparent radius of the Moon and Sun measured in degrees. It is unlikely that Aristarchus used these exact formulae, yet these formulae are likely a good approximation to those of Aristarchus. 
Aristarchus simplifiedEdit
I have a theory that great minds not only do much, they omit much. Suppose Aristarchus was more interested in knowing approximate facts and less interested in exact theories of geometry. Let's replace what he either knew, or should have known by the following facts:
 The angular size of the Moon and Sun are half a degree.
 The Earth's shadow (umbra) at the Moon's distance is twice the diameter of the Moon.
 The angle between the Sun and the Moon when visible Moon is 50% illuminated is effectively 90 degrees.
The third of these statements would have permitted Aristarchus to set the Sun at "infinity" (i.e. very far away), and used parallel lines to bypass a lot of complicated geometry (by "complicated" I mean too sophisticated for the average mind of a 21st century educated person.) Here is how Aristarchus might have concluded that the Earth is three times larger than the Moon (in diameter).
The distance to the Moon in Earth diametersEdit
Since one radian is 57.3 degrees, the distance to the Moon in Earth diameters can be written as:
Since the Moon is three times smaller than Earth, we have:
Solving, we obtain the distance to the Moon in Earth radii:
The accepted distance is closer to 60 Earth radii. Taking the ratio to extimate the percent error that Aristarchus would have made:
which corresponds to only a 30% error that Aristarchus might have made if only he understood the vast distance to the Sun.
Two more images re:AristarchusEdit
References and footnotesEdit
 ↑ It is almost entirely penumbra because the ball was held so that the angular size of the ball nearly equaled the angular size of the Sun. If the two angular sizes are equal, the umbra is essentially reduced to the area of a single point.
 ↑ We use a ballpoint pen that was rammed into the Styrofoam ball to hold it in place.
 ↑ Although our calculation stipulated a 120 inch rod, a more careful calculation indicated that 111 inches was closer to the condition that the angular size of the Styrofoam ball equals the angular size of the Moon.
 ↑ People interested in editing for Wikipedia should know about Inkscape because it is open source and makes the editable svg files preferred by Wikipedia and its "sisters".
 ↑ See also File:Solar eclipse lab on a sunny day 7 cropped.jpg
 ↑ Here the asterisk indicates that the cm* was as measured on a screen projected in the classroom. This forms a third scale. In this context, cm refers to the actual photograph.
 ↑ More properly, this shadow was 1.69 hatinches, since the hat is used on measurement made on the scale model.
 ↑ Another factor is that the student was not instructed to try for the largest possible shadow. After class, the instructor could discern a faint shadow 30 cm* in length on the screen that projected the image.