  The XMM-Newton Reflection Grating Spectrometer Team has obtained observations
ofa large number of coronal sources of various activity levels, ages, and
spectraltypes. In particular, X-ray bright RS CVn binary systems display
saturated coronal emission with spectral lines characteristic of hot (10-30 MK)
plasma. Furthermore, we have obtained XMM-Newton data from young solar analogs
both within and outside the X-ray saturation regime. We have simultaneously
analyzed the EPIC MOS and RGS data from these objects and have obtained coronal
abundances of various elements (e.g., C, N, O, Ne, Mg, Si, Fe). We show that
there is evidence for a transition from an Inverse First Ionization Potential
(FIP) effect in most active stars to a ``normal'' solar-like FIP effect in less
active stars. We discuss this result with regard to photospheric abundances.
