We consider a stationary , spherically outflowing wind consisting of electron-positron pairs and photons .
We do not assume thermal equilibrium , and include the two-body processes that occur in such a wind : Møller and Bhaba scattering of pairs , Compton scattering , two-photon pair annihilation , and two-photon pair production , together with their radiative three-body variants : bremsstrahlung , double Compton scattering , and three-photon pair annihilation , with their inverse processes .
In the concrete example described here , the wind injection source is a hot , bare , strange star .
Such stars are thought to be powerful sources of pairs created by the Coulomb barrier at the quark surface .
We present a new , finite-difference scheme for solving the relativistic kinetic Boltzmann equations for pairs and photons .
Using this method we study the kinetics of the wind particles and the emerging emission for total luminosities of L = 10 ^ { 34 } -10 ^ { 42 } ergs s ^ { -1 } ( the upper limit being set , at the moment , by computational limitations ) .
We find the rates of particle number and energy outflows , outflow velocities , number densities , energy spectra , and other parameters for both photons and pairs as functions of the distance .
We find that for L > 2 \times 10 ^ { 35 } ergs s ^ { -1 } , photons dominate the emerging emission .
For all values of L the number rate of emerging pairs is bounded : \dot { N } _ { e } \lesssim \dot { N } _ { e } ^ { max } \simeq 10 ^ { 43 } 
s ^ { -1 } .
As L increases from \sim 10 ^ { 34 } to 10 ^ { 42 } 
ergs s ^ { -1 } , the mean energy of emergent photons decreases from \sim 400 - 500 keV to 40 keV , as the spectrum changes in shape from that of a wide annihilation line to nearly a blackbody spectrum with a high energy ( > 100 keV ) tail .
These results are pertinent to the deduction of the outside appearance of hot bare strange stars , which might help discern them from neutron stars .