The Bigelow BA-330 has as much room as the bridge of The Enterprise and the Bigelow Genesis has as much room as a Humvee.
Wall Volume Mass Thickness (m^3) (tons) (m) Bigelow Genesis 11.5 1.36 .15 NASA Orion 19.6 8.91 Bigelow BA-330 330 23 .46 Space Station 837 450 .003
Bigelow habitats are lighter than NASA habitats and they have thicker walls. Thicker walls are helpful for defending against micrometeorites and radiation.
If artificial gravity is generated by spinning a spaceship, then according to en.wikipedia.org/wiki/Artificial_gravity, the spin period has to be at least 30 seconds for the inhabitants to not get dizzy. If we assume a spin period of 30 seconds and a gravity of 1 g,
Spin period = T = 2 π R / V = 30 seconds Spin radius = R = T2 A / (2π)2 = 228 meters Velocity = V = 2 π R / T = 48 meters/second Acceleration = A = V2 / R = 10 meters/second2
Suppose we use a tether to connect a spinning spaceship. Zylon is the material with the best tensile strength to density ratio.
Tether density = D = 1520 kg/m3 for Zylon Tether tensile strength = P = F / Ar = 5.8 GPa Mass of spaceship = M Radius of tether = R = T2 A / 4 pi2 = V2 / A Tether cross-section = Ar Mass of tether = m = 2 R Ar D Centripetal acceleration = A = 10 meters/second2 Tether tension force = F = M A Spaceship spin period = T = 2 π R / V = 30 secondsThe mass ratio of the tether to the spaceship is
m/M = 2 T2 D A2 / P / (4 π2) = 1.33e-6 T2 = .00119To be safe, the tether can be given a mass 10 times larger then this. Even so, the tether weighs much less than the habitable module, and so the mass of the tether is not a factor in the spaceship design.
If the spaceship mass is M=1000 tons, the tether mass is m=12 tons. Such a tether can easily be launched from the Earth.
For extremely large tethers you can use iron from the moon.
Atmosphere thicknes (tons/m2) Venus 1000 Titan 73 Earth, sea level 10 Earth, 12 km high 4.9 Mars .16 mSieverts Shielding thickness /year (tons/m2) Terrestrial radiation 2.02 n/a Average medical radiation .60 n/a Earth surface, cosmic rays only .39 10 Earth surface, all radiation 3.5 10 Earth 2 km altitude, cosmic rays only .9 8 Earth 3 km altitude, cosmic rays only 1.7 7 Earth 4 km altitude, cosmic rays only 3.3 6 Earth, 12 km altitude, equator 20 2.5 Earth, 12 km altitude, poles 100 2.5 Space station, 420 km altitude 150 .01 1/8 inch aluminum walls Space 600 .01 Space, 4 tons/m^2 shield 2.5 4 Mars surface 220 .16"Space" refers to interplanetary space between Earth and Mars.
At the space station, the Earth's magnetic field blocks 3/4 of the radiation from space.
The sun's magnetic field stops cosmic ray particles below 1 GeV.
The Earth's magnetic field deflects all but the highest-energy cosmic rays.
5 hour airplane flight incurs ~ .03 millisieverts.
A dose of 4800 millisieverts has a 50% risk of death.
The above data suggests that to shield against cosmic rays, you need at least 3 tons/meter2 of shielding.
Suppose a spherical spaceship is shielded with ice.
Radius of spaceship = r = 3 meters Radius of ice shield = R = 6 meters Density of ice shield = D = 1000 kg/meter3 Mass of ice shield = (4 &pi / 3) (R3-r3) = 792 tonsThe only way to get this much ice is from the moon. This is the source of the mass for the tether calculation.
The space station life support system:
1 liter of water per person per day
1 kg of food per person per day
Mass fraction in human body Oxygen .65 Carbon .18 Hydrogen .10 Nitrogen .03 Calcium .014 Phosphorus .011 Potassium .0025 Sulfur .0025 Sodium .0015 Chlorine .0015 Magnesium .0005 Iron .00006Air and water are the biggest challenges for life support in space. Water can be obtained from the moon and electrolysized to produce oxygen for air. Air also requires nitrogen, which cannot be found on the moon but is abundant in Mars' atmosphere.
The principal components of fertilizer are nitrogen, phosphorus, and potassium, with nitrogen being the heaviest component. Nitrogen can be obtained from Mars's atmosphere. If you want to grow crops on Mars you will have to bring phosphorus and potassium.
The most efficient way to grow plants in space is with aeroponics, where the roots are grown in open air. http://en.wikipedia.org/wiki/Aeroponics
Good locations for space bases are:
The L2 Lagrange point
Ice can be shipped from the moon to the other stations.
The L2 point stays tethered to the Earth as the Earth orbits.
The L2 point is ideal for telescopes because from there you can shield the sun, the Earth, and the moon all at the same time. The Webb telescope will go there. If we had a manned space station at L2 then we could assemble telescopes on-site and build colossal telescopes.
Cosmic rays consist mostly of high-energy protons with energies > 1000 MeV. When a proton passes through matter it loses energy from collisions with electrons and with nuclei. Electron collisions subtract a small amount of energy from the proton and nuclear collisions subtract most of the energy. This is because collisions with electrons are mediated by the electromagnetic force and collisions with nuclei are mediated by the strong force.
E = Proton energy L = Distance the proton travels through matter (meters) D = Density of the matter (kg/meter^3) V = Proton velocity C = Speed of lightProton kinetic energy is measured in MeV. 1 MeV = 1.6e-13 Joules. The rest energy of a proton is 1000 MeV.
Proton energy loss is governed by the "Bethe-Bloch" formula. For cosmic ray protons with E > 1000 MeV, the formula may be approximated as
EnergyLoss = 200 L (D/1000) MeVIf the proton is traveling through water with a mass density of 1000 kg/meter^3, the energy loss rate is 200 MeV/meter. The amount of matter required to stop a proton with E = 1000 MeV is 5 meters.
Spacecraft walls are thick enough to stop low-energy protons from the solar wind but they are of no help in stopping cosmic rays. Mars' atmosphere isn't thick enough either.
When a high-energy proton collides with a nucleus, most of the energy is lost in the collision, hence the transmission of protons through matter can be modeled as an exponential.
T = Initial intensity of protons t = Transmitted intensity of protons passing through a distance L of matter L = Distance the proton has traveled through the matter S = Characteristic stopping-length of the matter D = Density of the matter in kg/meter^3 A = Atomic number of the nuclei in the matter = 1 for protons = 8 for oxygen t = T exp(-L/S) S = .35 A^(1/3) (1000/D) metersFor oxygen, A = 8 and D=1000, hence the characteristic stopping length of protons in water is S = 0.2 meters.
Suppose you want to stop 99% of the protons.
t = .01 T L = 4.6 SIf water is used to stop cosmic ray protons, the formula predicts you need least 1 meter of it. This translates to a column density of 1 ton/meter^2.
This is an underestimate of the shielding required because when a high-energy proton hits a nucleus it creates a shower of secondary particles which must then be shielded. In practice, 4 meters of water are required. Muons are the biggest nuisance because they don't feel the strong force. Most of the cosmic radiation at the Earth's surface is from muons.
Dark matter particles rarely interact with matter. To observe a dark matter collision you have to screen out all background radiation, and so dark matter experiments are done deep underground to escape cosmic rays. Based on data from the web, how far undergound do you have to go?