  We present X-ray spectral analysis of 20 point-like X-ray sources detected in
Chandra Planetary Nebula Survey (ChanPlaNS) observations of 59 planetary
nebulae (PNe) in the solar neighborhood. Most of these 20 detections are
associated with luminous central stars within relatively young, compact
nebulae. The vast majority of these point-like X-ray-emitting sources at PN
cores display relatively "hard" ($\geq0.5$~keV) X-ray emission components that
are unlikely to be due to photospheric emission from the hot central stars
(CSPN). Instead, we demonstrate that these sources are well modeled by
optically-thin thermal plasmas. From the plasma properties, we identify two
classes of CSPN X-ray emission: (1) high-temperature plasmas with X-ray
luminosities, $L_{\rm X}$, that appear uncorrelated with the CSPN bolometric
luminosity, $L_{\rm bol}$; and (2) lower-temperature plasmas with $L_{\rm
X}/L_{\rm bol}\sim10^{-7}$. We suggest these two classes correspond to the
physical processes of magnetically active binary companions and self-shocking
stellar winds, respectively. In many cases this conclusion is supported by
corroborative multiwavelength evidence for the wind and binary properties of
the PN central stars. By thus honing in on the origins of X-ray emission from
PN central stars, we enhance the ability of CSPN X-ray sources to constrain
models of PN shaping that invoke wind interactions and binarity.
