How does electron degeneracy pressure prevent protostars with masses less than $0\mathrm{.}08M_{o.}$ from becoming main$-$sequence stars?

When electrons are too tightly packed, they exert an outward pressure opposing further gravitational collapse in the core.

It causes electrons to move more quickly increasing the temperature of the core.

It raises the density of the core, accelerating the gravitational collapse of the protostar.

It causes the protostars smaller than $0\mathrm{.}08M_{o.}$ to fuse its core hydrogen too quickly, before it can become a mainsequence star.