Terraforming a Planet

This is a work in progress.
I'll gladly accept contributions.

Stage 1: Information gathering
It's important to gather as much accurate information as possible. Without it you risk failure, and the destruction of an entire world.

Important information you will need to know:

Questions to answer:

Stage 2: Determine the best course of action
This stage determines what will need to be done and when to do it.
Note: the availability of a resource is not limited to the planet. A resource can come from anywhere, depending on it's economic, technological and physical feasibilities. It may already be available on the planet, or from a moon, asteroid belt, interplanetary medium, interstellar medium, gas giant, another planet, or another stellar system.

0Is there life already on the planet?
Nogo to 1
1Is there enough N2 available for an Earth-standard atmosphere?
Yesgo to 2
2Is there enough Oxygen available to "water" the planet and for an Earth-standard atmosphere?
Yesgo to 3
3Is there enough Hydrogen-1 available to "water" the planet?
Yesgo to 4
4Determine the H-value from Equation 1
H-value > 2 : the planet has too much gravitygo to 5
H-value <= 2, H-value > 1 : gravity is acceptablego to 8
H-value = 1 : the planet has an "ideal" gravitygo to 8
H-value < 1 : the planet cannot hold Hydrogen-1go to 6
5Atmospheric pressure (Po)
Po > 1 Earth-standard atmosphereAction 1 then go to 4
Po <= 1 Earth-standard atmosphereAction 2 then go to 4
6Determine the additional mass (x) needed from Equation 2
x >= original mass. The planet cannot be terraformed stop
x < original mass. The planet can be terraformedgo to 7
7Is there enough additional mass (x from 6) available?
YesAction 4 then go to 1
8Atmospheric Temperature (T)
T > 300 KAction 5 then go to 4
T <= 300 K, T >= 275 Kgo to 9
T < 275 KAction 6 then go to 4
9Atmospheric pressure (Po)
Po > 1 Earth-standard atmosphereAction 7 then go to 4
Po = 1 Earth-standard atmospherego to 10
Po < 1 Earth-standard atmosphereAction 3 then go to 4
10Is the atmosphere breathable by humans?
YesAction 8 then go to 11
NoAction 9 then go to 4
11Has a strong Ozone (O3) layer formed around the planet?
Yesgo to 12
NoAction 10 then go to 8
12Is the partial pressure of O2 below 25 kPa?
Yesgo to 13
NoAction 11 then go to 4
13Is background radiation at acceptable levels?
Yesgo to 14
NoAction 12 then go to 1
14Is cosmic radiation at acceptable levels?
Yesgo to 15
NoAction 13 then go to 15
15Colonisation can begin!Action 14

Action list

Action 1
Remove all but one Earth-atmosphere from the planet. The excess atmosphere can be transported from the planet and dumped on a frozen moon, in the outer system, for later use.

Action 2
Remove mass from the planet. The planet should be mined for high-density metals. Silicates should also be removed if the mantle is too thick. The excess mass is transported from the planet. It could be used to form an orbiting moon, or as a resource to terraform other planets in the system.

Action 3
Add N2 to the atmosphere until one Earth-atmosphere is achieved.

Action 4
Add additional mass to the planet. Ensure the mass is:

Action 5
Decrease the atmospheric temperature. This can be partially achieved through Action 7.
Additional methods include: Carbonate and sulfate minerals will begin to form when the atmospheric temperature drops below a critical temperature. The critical temperature is dependant on the surface geology and the mineral. This will slowly remove some CO2 and SO2 from the atmosphere.
Note: Shading the planet with large reflective mirrors is not a good idea. The reflected light will generate a force pushing the mirrors into a lower orbit, and eventualy burn up in the atmosphere and crash to the surface.

Action 6
Increase the atmospheric temperature.
Methods include: Action 7
The atmospheric gases should be compressed and stored. The gases can be stored in reflective cylinders, on the surface or in orbit. When conditions are favourable the gases can be distilled and stored seperately. CO2 and SO2 can be ionised. The Carbon and Sulfur can be stored and the O2 released or stored seperately.
Note: As atmospheric pressure decreases, the planets mantle will expand. Deep rifts will open in the surface and mountains will slowly push up. Volcanic activity will increase and lava flows will initially become more common. The expansion of the mantle will slightly increase the planetary radius and surface area. This expansion will slightly decreased atmospheric pressure, but not enough to generate a positive feedback loop. The atmosphere in the rifts will be more dense than at the radius, and contribute towards lowering atmospheric pressure.

Action 8
Water is now added to the planet. H2 and O2, in a 2:1 ratio, is slowly released into the atmosphere. If H2 and O2 are available as stored gases then they should be used first. When the stored supply is exhausted, H2 and O2 should be imported.
Note: bodies of water will form in depressions and at low elevations. These areas should be evacuated in advance.
Note: an increase in surface water will decrease the planetary albedo and in turn increase the greenhouse effect. However, convection currents will form in the atmosphere, allowing the planet to better regulate it's temperature.
Note: CO2 and SO2 will dissolve in water. This will initially remove some of the CO2 from the atmosphere, allowing it to cool. The presence of water will also increase the rate of formation of Carbonate and Sulfate minerals.

Action 9
The atmospheric constituents must be replaced, converted or exchanged with breathable consitituents. Stored gases should be used where possible. If stored gases are not available then imported gases are used.

Action 10
Colonisation cannot begin until a strong Ozone (O3) layer has formed. Additional O2 released into the atmosphere and complete removal of all ozone-depleting gases will accelerate the formation of ozone.

Action 11
Organic material will spontaneously combust around 25kPa. Reduce the concentration of O2 in the atmosphere by releasing H2.

Action 12
Colonisation cannot begin until background radiation is at acceptable levels. The source of the radiation will need to be determined. Radon (Rn) gas or long-life radioactive elements can be stored in sheilded locations, or transported off the planet. Colonisation can wait until short-life radioactive elements decay naturally.

Action 13
Colonisation may be limited to lower elevations. If the cosmic radiation levels are too high at lower elevations then the planet may not be colonisable, or habitats may need to be insulated or subterranean.

Action 14
Plants are added to the planet. The weather, atmospheric pressure; temperature; and constituents will fluctuate significantly. All possible resources will need to be transported to the planet and stored in advance, either in orbit or on the planets surface.
The colonists will be responsible for maintaining a balance by: