## Pair Density in Supergiant Stars.

Hi,

I'm curious about the electron-positron pair density at the very center
of an exhausted supergiant star just prior to the point of catastrophic
collapse (i.e. in the final moments of hydrostatic equilibrium after all
fusion steps have gone to completion).

I know pair production will be suppressed in lower mass supergiant stars
by electron degeneracy. What I'm curious about is the pair density in
higher mass stars that have higher temperature and lower density in the
core, and hence less degeneracy. In particular I'm interested in the
pair density for stars in which core collapse will primarily be
triggered by photoexcitation and photodisintegration (as opposed to
electron capture) when the temperature is approximately 8.0 * 10E9 K,
and the density is a pproximately 3.0 * 10E9 g/cm3.

Thank You
Rev. Thomas Winans D.D.