Central stars of PN (CSPN) are difficult to study because of their faintness in the visible (due to their high temperature) and the contamination of their spectra by nebular emissions. Unlike stars on the main sequence (MS), for which there exists a unique relationship between mass and effective temperature, CSPN undergo considerable changes in temperature over their short lifetimes. Although their masses do not change significantly, their surface abundances do change as the result of nuclear burning and mass loss. Assuming that the stellar winds from the CSPN are driven by radiation pressure, the mass-loss rate is mainly a function of T* and surface gravity (log g). In this case, the spectral classification of central stars can in principle be determined by three parameters: effective temperature, surface abundance, and wind strength. In this chapter, we discuss these three parameters in turn.

Determination of the temperature of the central star

Zanstra temperature

Zanstra (1927) developed the method to derive the central star temperature by comparing the nebular recombination flux with the stellar continuum magnitude. This method is based on the assumption that the number of Lyman continuum photons absorbed in the nebula is equal to the total number of recombinations to all levels excluding the ground state. Harman and Seaton (1966) used the nebular Hβ flux to estimate the total number of Lyman continuum photons, and they derived T* by comparing the Hβ flux with the stellar V magnitude.