This page builds the toolbox. The parent note throws around symbols like v, ρ, σ, Q∗, and phrases like "stagnation point" and "σT4". If any of those looked like magic runes, this page turns them into pictures. We go in order, so each idea leans on the one before.
The picture: an arrow along the flight path. The length of the arrow is the speed. A longer arrow means more distance covered each tick of the clock.
Why the topic needs it: every heating formula depends on v — and dangerously so. As we build up to the convective heating law in section 6, we will see the heat scale as v3, meaning doubling the speed multiplies the heating eightfold.
Why the 21v2 and not just v? Because energy is what it takes to stop the motion, and stopping something twice as fast costs four times as much work — the v2 captures that. Try it: pushing against a wall twice as hard over twice the distance is four times the effort.
The picture: imagine slicing the vehicle into 1-kg cubes. Each cube carries the same ek. This lets us talk about heating "per kg of shield" without knowing the total mass.
Worked number (matches the parent): at v=7800 m/s,
ek=21(7800)2=3.042×107J/kg≈30MJ/kg.
The prefix M (mega) means one million, so 30 MJ =3.0×107 J. That is the "terrifying" number: about four times the energy needed to boil away a kilogram of steel.
See Specific Impulse and Energy Budgets for where this "per kilogram" bookkeeping comes from.
The picture: a box one metre on each side. Count the air molecules inside it and weigh them — that weight is ρ. A crowded box = high density; a nearly empty box = low density.
Why the topic needs it: the heat the vehicle feels depends on how much hot gas is thrown at it each second, and that is set by ρ. As we will see in section 6, the convective heating combines ρ and v into a product ρv3 that peaks at a middle altitude — high up there is too little air (ρ small), low down the vehicle has already slowed (v small). We meet that product properly once its formula is on the table.
The picture: below, a fat rounded nose (large Rn) versus a pointy nose (small Rn), each with the biggest circle that fits.
Why the topic needs it: the stagnation-point heating scales as 1/Rn — a bigger, blunter nose lowers heating. We explain why in section 6, right after the convective-flux symbol is defined. This single fact explains why reentry capsules are round bowls, not arrows. Details live in Blunt Body Aerodynamics.
The picture: a curved shock standing off the nose like a bow-wave in front of a boat. Between the shock and the wall is the glowing shock layer. The centreline hits the wall at the stagnation point.
More in Bow Shock and Stagnation Point and Reentry Aerothermodynamics.
The picture: shine a heat lamp on a stamp-sized patch of the shield. q˙ is how brightly that patch is being cooked; q˙conv is the share of that cooking done by hot gas scrubbing against the surface.
Why the fourth power T4 and not just T? Because radiated power grows ferociously with temperature — this is measured, not chosen, and captured by the Stefan–Boltzmann law. It is the reason a glowing tile can dump enormous heat back out: doubling T multiplies the radiated heat by 24=16.
The picture: the same tile at rising temperature glows dull red, orange, then white — and the arrows of escaping light thicken far faster than the temperature climbs.
The full story is in Radiative Heat Transfer and Stefan–Boltzmann Law.
Every box carries a symbol you now own, spelled the same way as in the text: q˙conv is "q_conv", q˙rad is "q_rad", and m˙ is "m dot". The parent note's formulas are just these boxes wired together.