  To date, pulsational variability has been measured from nearly 70 DBVs and
500 DAVs, with only a fraction of these having been the subjects of
asteroseismic analysis. One way to approach white dwarf asteroseismology is
forward modeling, where one assumes an interior structure and calculates the
model's periods. Many such models are calculated, in the search for the one
that best matches an observed period spectrum. It is not computationaly
manageable, nor necessary, to vary every possible parameter for every object.
We engage in a systematic study, based on a sample of 14 hydrogen atmosphere
white dwarfs, chosen to be representative of the types of pulsation spectra we
encounter in white dwarf asteroseismology. These white dwarfs are modeled with
carbon and oxygen cores . Our goal is to draw a connection between the period
spectra and what parameters they are most sensitive to. We find that the
presence of longer period modes generally muddies the mass and effective
temperature determinations, unless continuous sequences of l = 1 and l = 2
modes are present. All period spectra are sensitive to structure in the helium
and hydrogen envelope and most to at least some fatures of the oxygen abundance
profile. Such sensitivity can be achieved either by the presence of specific
low radial overtone modes, or by the presence of longer period modes.
Convective efficiency only matters when fitting periods greater than 800 s. The
results of this study can be used to inform parameter selection and pave the
way to pipeline asteroseismic fitting of white dwarfs.
