  We present Chandra X-ray observations of 6 previously-identified Peter Pan
objects, rare 40 Myr systems with evidence of primordial disk retention. We
observe X-ray luminosities (0.8-3.0 keV) ranging from log Lx 27.7-29.1. We find
that our Peter Pan sample exhibits X-ray properties similar to that of
weak-lined T-Tauri stars and do not exhibit evidence of stellar accretion
induced X-ray suppression. Our observed Peter Pan X-ray luminosities are
consistent with that measured for field dM stars of similar spectral type and
age, implying their long primordial disk lifetimes are likely not a consequence
of unusually faint X-ray host stars. Our derived X-ray photoevaporative mass
loss rates predict our systems have passed the point of rapid gas dispersal and
call into question the impact of this internal mechanism for primordial disk
dispersal around dM stars. Our qualitative assessment of the surrounding Peter
Pan environments also does not predict unusually low levels of external
photoevaporation relative to other respective moving group members. Overall,
our results suggest Peter Pan disks may be a consequence of the low FUV flux
incident on the disk in low-mass DM stars given their relatively lower levels
of accretion over the course of their pre-main-sequence evolution.
