The surface of airless worlds will be exposed to radiation so it's likely the inhabitants would live underground.

Moreover, it is not as hard to burrow. The deepest gold mine on earth goes down about 4 kilometers. The heat and immense pressure make it hard to dig deeper. In contrast, the entire volume of a small body can be reached.

Courtney Seligman shows how to compute the pressure of a body with uniform density. The bodies we look at don't have uniform density but we'll use his method as a first order approximation.

Central pressure of a spherical body with uniform density is 3 g

^{2}/(8 π G)

Where G is universal gravitation constant, g is body's surface gravity and R is body's radius.

At distance r from center, pressure is (1 - (r/R)^2) * central pressure.

What is the pressure 4 kilometers below earth's surface?

Earths's radius R is 6378000 meters. r is that number minus 4000 meters. g is about 9.8 meters/sec^2.

Plugging those numbers into

(1 - (r/R)^2) * 3 g

^{2}/(8 π G)

gives

**2120 atmospheres**.

Besides pressure, heat also discourages us from burrowing deeper. So it might be possible to dig deeper on cooler worlds but for now

**we'll use 2120 atmospheres as the limit**beyond which we can't dig.

3/(8 π G) * g * R

^{2}gives different central pressures for various worlds:

Ceres center is 1430 atmospheres, well below our 2120 atmosphere limit. And Ceres is a cooler world than earth. We would be able to tunnel clear through the largest asteroid in the main belt. Since smaller asteroids would have smaller central pressure, we would be able to tunnel through the centers of every asteroid in the main belt.

Imagine a mohole going from a body's north pole to south pole:

The diagram above breaks the acceleration vector into vertical and horizontal components. The mohole payload has the same vertical acceleration components as an object in a circular orbit with orbital radius R, R being body radius.

Somone jumping into this mohole could travel to the opposite pole for zero energy. Trip time would be the orbital period: 2 π sqrt(R

^{3}/μ).

Other chords besides a diameter could be burrowed. I like to imagine 12 subway stations corresponding to the vertices of an icosahedron:

The red subway lines to nearest neighbors would correspond to the 30 edges of an icosahedron .

Green subway lines to the next nearest neighbors would correspond to the 30 edges of a small stellated dodecahedron.

And there could be 6 diameter subway lines linking a station to stations to their antipodes.

The energy free travel time of all these lines would be the same as the diameter trip time:

2 π sqrt(R

^{3}/μ).

It would be possible have a faster trip time than 2 π sqrt(R

^{3}/μ). A train could be accelerated during the first half of the trip and decelerated the second half. During the second half, energy could be recovered using regenerative braking.

Most of small bodies in our solar system have internal pressures that don't prohibit access. But in some cases central pressure exceeds 2120 atmospheres. We'd be able to burrow only so deep. Here's my guesstimate of the maximum depth for various bodies:

Luna 40 kilometers

Mars 15 kilometers

Ganymede 77 kilometers

Callisto 97 kilometers

Europa 55 kilometers

Titania 318 kilometers

Oberon 61 kilometers

Pluto 200 kilometers

Haumea 82 kilometers

Eris 108 kilometers

Here is the spreadsheet I used to look at internal pressures.

The top four kilometers of earth's surface is only a tiny fraction of the accessible mass in our solar system.

## 9 comments:

Question; for the asteroid example, did you vary the g force from Earth normal? The figure of over 1400 atmospheres seems a bit too high.

Ceres surface gravity is .28m/s versus Earth's 9.8 m/s. Ceres mean radius is 476.2 km versus Earth's mean radius of 6371 km.

Charles, it's possible I made an error. Checking my spreadsheet...

I have 476000 meters as Ceres' radius. 9.43e20 kg. I get a surface gravity of .278 meters/sec^2. These figures seem fairly close to yours.

What about the Coriolis effect for all the cases besides the transpolar hole ? I guess they would require curved tunnels.

Good observation jesrad! Googling Coriolis force...

http://en.wikipedia.org/wiki/Coriolis_effect#Formula says coriolis acceleration is -2W X V where W is the angular velocity vector.

I'll imagine a tunnel going from an equatorial point to equatorial point. That makes it simpler--the angle between W and V is 90º and sin(90º) is 1. So the coriolis acceleration becomes simple -2WV.

The sidereal day of Ceres is .378 days. 2 pi/(.378 days) comes to an angular velocity of .0001924 radians per second.

Our subway car would be moving fastest at Ceres' center, .3659 km/s if we're letting gravity do all the work.

-2WV would come to -.14 meters/sec^2 if I did my arithmetic right. (It's a good idea to check my arithmetic, I occasionally make mistakes).

About 1/70 of a g. That's a pleasant surprise, I was thinking coriolis acceleration would be high in the rapidly spinning asteroids.

Jupiter's moons Metis and Adrastea have an orbital period of about .3 days. The other moons are slower with the slowest Callisto having an period of about 17 days.

For Saturn the moons range from Mimas (about a day) to Titan which has an approximately 16 day orbit.

What about friction?

Doug, of course friction can't be entirely eliminated. However if the tunnel is airless and coriolis is a small fraction of a g, I believe friction loss could be small.

To eliminate friction something like this would be useful.

http://en.wikipedia.org/wiki/Inductrack

It would also make sure that Coriolis effect wouldn't make the subway car hit the side of the tunnel.

There is a problem with your equation; the units don't work out. G has units of N m^2/kg^2. Gravity has units of N/kg. R has units of m. And pressure has units of kg/m^2; if the equation is correct, then the final units will be kg/m^2.

But 3/(8 π G) * g * R2 has units of kg:

1/(N m^2/kg^2)*(N/kg)*(m^2)

= (N/kg)*(m^2)/(N m^2/kg^2)

= (N m^2 kg^2)/ (N m^2 kg)

= kg

This is also seen in your central pressures which are wrong. See

http://cips.berkeley.edu/events/rocky-planets-class09/ch6_depater_lissauer.pdf.obscure

Which gives the central pressure of a planet as (3 G M^2)/(8 pi R^4)

Anonymous, pressure is measured in pascals. This unit is kg/(m*s^2), not kg/m^2.

However you're correct that my expression gave kilograms. When checking Dr. Seligman's page I see here term for surface gravity is gR. The R's supposed to be subscripted.

I mistakenly interpreted gR^2 as g*R^2.

I've corrected my text. Now I am simply using g for surface gravity. I will check my spreadsheet when I have the time.

Thanks for the heads up.

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