Abstract
Collisional excitation of the 21 cm hyperne transition is not strong enough to thermalize it in warm neutral (\intercloud) interstellar gas, which we show by simultaneously solving the equations of ionization and collisional equilibrium under typical conditions. Coupling of the 21 cm excitation temperature and local gas motions may be established by the Ly- radiation eld, but only if strong Galactic Ly- radiation permeates the gas in question. The Ly- radiation tends to impart to the gas its own characteristic temperature, which is determined by the range of gas motions that occur on the spatial scale of the Ly- scattering. In general, the calculation of H I spin temperatures is a more dicult and interesting problem than might have been expected, as is any interpretation of H I spin temperature measurements.
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