  Measurement of distances and moments of inertia of pulsars must be useful,
for instance, for three-dimensional mapping of the dispersion and rotation
measures, constraining the nuclear equation of state, etc. The distances and
moments of inertia can be measured by fitting the gamma-ray lightcurves of
pulsars, because the gamma-ray emission seems to be governed by easily
calculable physics. The (first-principle) theoretical lightcurves have been
computed only for weak pulsars (pair production near the light cylinder much
smaller than Goldreich-Julian [1] per rotation), and at insufficient accuracy;
but, since this computation has been done by a self-taught numericist, it must
be possible to improve the theoretical accuracy for weak pulsars, and also to
extend the computation to non-weak pulsars.
  To invite the computational effort of better-equipped researchers, we
describe an (entirely obvious) procedure for measuring the distances and
moments of inertia for weak pulsars.
