Pat's Blog and Random Notes

What If The Moon ...

Here's a video showing what the Moon would look like if it were as close to Earth as the International Space Station is.

The io9 article quickly points out that if the Moon were that close, it would break apart and form a ring (like Saturn's) because of the Roche limit. Here's another io9 article with pictures of what that would look like.


But here, let's assume the Moon doesn't break apart. Here's a bird's-eye view looking down at the north pole at the moment when both the ISS and the Moon are about to rise over the horizon.

Show Instructions

Show Instructions

  • Hit the “Press Play” button on the bottom left corner to start and stop the animation.
  • Use the “Reset” button on the top right corner to restart the animation from the beginning. It takes a few seconds to reload. Be patient.
  • You can move the Moon and the ISS manually without playing the animation.
  • On my computer, the animation consumes about 25% more CPU cycles when it's running. Don't forget to pause it before you continue reading the article.

GeoGebra Dynamic Worksheet

Patrick Truchon, 19 October 2013, Created with GeoGebra

Note that:

  • All the distances are to scale (the size of Earth, Moon, the orbits).
  • The animation runs about 60 times faster than real life so that one second of animation is one minute of real time. The clock on the top right corner helps keep track of time.
  • The changing darker shade on the Moon when it flies by represents the visible part of the Moon since the rest is hidden behind the Moon's curvature. It has nothing to do with sunlight.

Now let's try to answer a few interesting questions…

Period of Revolution

Why is the ISS going faster if the Moon is at the same distance?

Even though the surface of the Moon is 420 km away from the surface of the Earth (like the ISS), its centre of mass isn't, which means it's in a different orbit. It's not taking more time to go around because it's bigger and more sluggish. If that were true, the astronauts in the ISS would want to orbit faster than the station itself. That would be weird…

The only thing that affects orbital speed is the distance from the planet. The further away an object is, the longer it takes to go around it. For example, Neptune takes about 165 human years to go around the sun because it's so much further away from it than we are.

So because the Moon's centre of mass is further away, it revolves around the Earth more slowly:

Period of Revolution
ISS 1 hr 33 min
Moon 2 hr 11 min

Show Calculations

Show Calculations

To do these calculations, we'll need some (but not all) of the following numbers. Can you think of which one(s) we don't need?

Radius Mass
Earth 6370 km = 6.37 x 106 m 5.97 x 1024 kg
Moon 1740 km = 1.74 x 106 m 7.35 x 1022 kg
ISS 72.8 m x 108.5 m x 20 m 4.5 x 105 kg
Distance to Surface 420 km = 4.2 x 105 m

The orbital period $T$ is the time (in seconds) it takes to go around the planet. To find it, we start by setting the gravitational force equal to the centripetal force:

$$ \frac{GMm}{r^2} = \frac{mv^2}{r} $$

Here's what all those variables mean:

  • $G$ = 6.67 x 10-11 N·m2/kg2 is the universal gravitational constant. We usually call it “big gee”.
  • $M$ is the mass of the planet (or star).
  • $m$ is the mass of what orbits around. Notice how $m$ cancels in this equation. It means that the mass of the orbiting object has no effect on the speed at which it orbits. Again, lucky for the ISS astronauts!
  • $r$ is the distance (radius) between the centre of mass of the planet (or star) and that of the orbiting object.
  • $v$ is the tangential speed of the orbiting object. That is, it's the speed, parallel to the surface, at which the object is flying.

$v$ can calculated by taking the total distance around the Earth (the circumference of a circle) divided by the period of revolution, $T$, which is what we're really after:

$$v = \frac{2\pi r}{T}$$

Thus, the previous equation becomes:

$$ \frac{GMm}{r^2} = \frac{m}{r}\left(\frac{2\pi r}{T} \right)^2 $$

Simplifying and solving for $T$, we get:

$$ T = 2 \pi \sqrt{\frac{r^3}{GM}}$$

Again, notice that the only mass that matters is that of the Earth, not the Moon or the ISS.

So for the ISS, the orbital period is:

$$ T = 2 \pi \sqrt{\frac{(6.37\times 10^6 + 4.2\times 10^5)^3}{(6.67 \times 10^{-11})(5.97 \times 10^{24})}} = 55\underline{7}1 \text{ sec} = 92.\underline{8}5 \text{ min}$$

And for the Moon, it's:

$$ T = 2 \pi \sqrt{\frac{(6.37\times 10^6 + 4.2\times 10^5 + 1.74\times 10^6)^3}{(6.67 \times 10^{-11})(5.97 \times 10^{24})}} = 78\underline{4}4 \text{ sec} = 13\underline{0}.7 \text{ min}$$

The reason I've underlined some digits is because they are the last significant ones. I kept a few digits afterwards so I can reuse these results in subsequent calculations without accumulating rounding errors.

Flyby Duration

How long would we see them in the sky?

Since the Moon would take about twice as long to go around the Earth as the ISS, it's reasonable to think that it would be visible for about twice as long. But that close to Earth, the Moon's size is very big, and if we calculate the time from when we “start” seeing it to the time when we completely lose it below the horizon, we would see it four times longer than we'd see the ISS!

At best (if they rise straight over us, and ignoring atmospheric and optical issues):

Visible for at most
ISS 10 min and 30 sec
Moon 41 min and 30 sec

Show Calculations

Show Calculations

We know how long it takes for the ISS and the Moon to go around Earth (360°). Now, we need to find the fraction of their orbit when they are above the horizon.


If we draw a right triangle from the centre of the Earth to the ISS and to us, we see that

  • the vertical side of the triangle is the radius of the Earth (6370 km)
  • and the hypotenuse is the radius of the ISS's orbit (6370 km + 420 km = 6790 km)
  • The angle of this right triangle is:

    $$\cos^{-1}\left(\frac{6370}{6790}\right) = 20.258^{\circ}$$

  • Which means the fly by duration is:

    $$ \frac{(2)(20.258^\circ)}{360^\circ} 92.\underline{8}5 \text{ min} = 10.\underline{4}4 \text{ min}$$

The Moon

For the Moon, it's a bit more complicated since we can't treat it as a point (like the ISS). Instead, we have to find out where the Moon's centre is when its tip breaks above the horizon.

  • To find the vertical leg of the right triangle, we subtract the Earth's and the Moon's radii: 6370 km - 1740 km = 4630 km.
  • To find the hypotenuse of the triangle, we add the Earth's radius with the surface distance and the Moon's radius: 6370 km + 420 km + 1740 km = 8530 km
  • Then, the angle of this right triangle is:

    $$\cos^{-1}\left(\frac{4630}{8530}\right) = 57.126^{\circ}$$

  • Which means the fly by duration is:

    $$ \frac{(2)(57.126^\circ)}{360^\circ} 13\underline{0}.7 \text{ min} = 41.\underline{4}8 \text{ min } $$

Apparent Size

I've seen the video, but how do you explain how it would “look” like?

During its flyby, the following three aspects change:

  • The Moon's distance from us.
  • The angular size of the Moon.
  • The surface area of the Moon that we can see.

At the horizon Overhead
Distance from us 1425 km 420 km (3.4x closer)
Angular size 66.7° 107.3° (1.6x more)
Visible surface area 22.5% 9.7% (2.3x less)

Distance From us

Because the Moon is about 3.4 times closer to us when it's overhead compared to when it's at the horizon, we'd see craters getting bigger and bigger as the Moon rises.

Angular Size

As soon as the Moon is completely over the horizon, what we see would cover about 67° of our field of vision. To put this number into perspective, looking at the horizon and then looking straight up covers 90°. If the Moon was rising right behind the Eiffel tower (which is 300 m high), you'd only have to be 129 m away from the tower to see the Moon at the same eight as the tower.

As the Moon rises, the disk that we see in the sky would grow in angular size to 107° (1.6 times more). This is crazy! It means that looking at the horizon, we would only be able to see 36° of sky before we see the Moon. In every direction! It would be like being in a room where the ceiling is the Moon and the walls are open.

Sufrace Area

As soon as the Moon is completely over the horizon, we would see about 23% of its surface area (instead of about 50% for our real Moon).

However, as it rises straight overhead, what we see would drop to 9.7% (2.3 times less). That's because as it gets closer to us, more of the Moon's surface gets hidden behind its curvature.

Show Calculations

Show Calculations

Visible Surface Area

Before calculating specific cases, we need to derive a general formula for calculating the percentage of visible surface area as a function of the angle.

  • Let's start by rotating the Moon so that the visible part is pointing to the right.
  • Next, we draw an infinitesimally small strip on the surface that goes all the way around (in green).
  • That strip is essentially a very thin rectangle wrapped around. Its length is $2\pi r$ and its width is $R d\theta$
  • The area of that strip is thus: $dA = (2 \pi r)(R d\theta)$
  • As $\theta$ changes, $r$ changes as such: $r = R\sin\theta$
  • So the area element is: $dA = (2 \pi R\sin\theta)(R d\theta) = 2 \pi R^2 \sin\theta d\theta$
  • To find the total visible area, we integrate between 0 and the final angle $\theta$:

$$A(\theta) = \int_0^\theta 2 \pi R^2 \sin\theta' d\theta'$$

$$ = 2 \pi R^2 \int_0^\theta \sin\theta' d\theta'$$

$$ = 2 \pi R^2 \cos\theta \Big|_\theta^0$$

$$ = 2 \pi R^2 (1 - \cos\theta)$$

  • Let's test it. We know that the total surface area of a sphere is $4\pi R^2$. According to our formula, we need θ = 180° to cover the whole circle: $ A = 2 \pi R^2 (1 - \cos(180^\circ)) = 2 \pi R^2 \big(1 - (-1)\big) = 4 \pi R^2$
  • So the percentage of the surface area we see is given by:

$$ 100\% \times \frac{A(\theta)}{A_\text{sphere}}  = 100\% \times \frac{2 \pi R^2 (1 - \cos\theta)}{4 \pi R^2} $$

$$ =  50\% \times (1 - \cos\theta)$$

At The Horizon:

The first step is to find all sides and angles of this right triangle.

  • To find the horizontal side, we start by finding the coordinates of the Moon's centre.
    • Since it's right above the horizon, the y-coordinate is $6370 + 1740 = 8110$
    • Then we use the equation of the Moon's orbit to find the x-coordinate:

      $$ x^2 + y^2 = (6370 + 420 + 1740)^2 $$

      $$ x^2 + (8110)^2 = (8530)^2 $$

      $$ x = 26\underline{4}3.6$$

  • The hypotenuse of the triangle is $\sqrt{1740^2 + 26\underline{4}3.6^2} = 31\underline{6}4.9$
  • This means that the closest point of the Moon is 3164.9 km - 1740 km = 1424.9 km from us.

Next we find the angles:

  • The angle at “You Are Here” is:

$$\tan^{-1}\left( \frac{1740}{2643.6} \right) = 33.35^\circ$$

  • So the angular size is double: 66.7°
  • And the angle at the centre of the Moon is 90° - 33.35° = 56.65° so the percentage of the surface we see is: $50\% \big(1 - \cos(56.65°)\big) = 22.5 \%$


The same calculations are much simpler in this case.

  • The hypotenuse is simply 1740 km + 420 km = 2160 km and we don't need the other side.
  • The angle at “You Are Here” is:

    $$\sin^{-1}\left( \frac{1740}{2160} \right) = 53.66^\circ$$

  • So the angular size is double: 107.3°
  • And the angle at the centre of the Moon is 90° - 53.66° = 36.34° so the percentage of the surface we see is: $50\% \big(1 - \cos(36.34°)\big) = 9.7 \%$

Coming Up Next

That's it for this weekend. Here are a few more ideas I have sketched on scrap paper that I want to add (maybe next week).

What About Gravity?

Here, I'll find out if how much lighter the moon fly by would make us feel.

I'll also look at it from the perspective of an astronaut on the moon. That part will be fun since the moon is revolving so fast!

Spoiler Alert

Spoiler Alert

On Earth, gravity would increase by 0.2% when the Moon is on the other side of the Earth, and it would decrease by 0.7% when the Moon is straight overhead. I can't even start to imagine how that would affect the tides though… Maybe it would revolve too fast?

On the Moon however it's a very different story! Assuming that the Moon is still tidally locked, we'll see that an astronaut on the “far side” of the Moon would barely be able to stay on the surface, but an astronaut on the “near side” would fall towards Earth. Although, I don't know if they'd fall *on* Earth or into a lower orbit…

And Sun Light?

I want to see if I can add sun rays to the Geogebra animation so that we can see which part of the moon would be lighted and which part of Earth would be in Moon's umbra depending on the time of day.

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