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We present X-ray spectral analysis of 20 point-like X-ray sources detected inChandra Planetary Nebula Survey (ChanPlaNS) observations of 59 planetarynebulae (PNe) in the solar neighborhood. Most of these 20 detections areassociated with luminous central stars within relatively young, compactnebulae. The vast majority of these point-like X-ray-emitting sources at PNcores display relatively "hard" ($\geq0.5$~keV) X-ray emission components thatare unlikely to be due to photospheric emission from the hot central stars(CSPN). Instead, we demonstrate that these sources are well modeled byoptically-thin thermal plasmas. From the plasma properties, we identify twoclasses of CSPN X-ray emission: (1) high-temperature plasmas with X-rayluminosities, $L_{\rm X}$, that appear uncorrelated with the CSPN bolometricluminosity, $L_{\rm bol}$; and (2) lower-temperature plasmas with $L_{\rmX}/L_{\rm bol}\sim10^{-7}$. We suggest these two classes correspond to thephysical processes of magnetically active binary companions and self-shockingstellar winds, respectively. In many cases this conclusion is supported bycorroborative multiwavelength evidence for the wind and binary properties ofthe PN central stars. By thus honing in on the origins of X-ray emission fromPN central stars, we enhance the ability of CSPN X-ray sources to constrainmodels of PN shaping that invoke wind interactions and binarity.

The Chandra Planetary Nebulae Survey (ChanPlaNS): III. X-ray Emission from the Central Stars of Planetary Nebulae