It is bona-fide knowledge that, radiative feedback from the core of a pre-main sequence (PMS) star leads to a global accretion delay in stellar formation. How long the accretion delay lasts, remains poorly constrained in existing numerical and analytical model. This problem is more common in massive star formation where the global accretion delay leads to modulated accretion rates which effectively traps massive stars in a pre-ignition bottleneck, where they exhaust their energy supply before achieving stable nuclear fusion. Numerical tools capable of this task are lacking at present. We consider the present investigation an important step in this direction. Here we show that, in a radiative pressure-dominated regime, an unprecedented radiative contraction delay $t_{text{RD}}$, must exceed the Kelvin-Helmholtz timescale ($t_{text{KH}}$). This uncertainty poses a major stumbling block in our current understanding of stellar evolution.