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The Wide-field Imager for Parker Solar Probe (WISPR) captures unprecedentedwhite-light images of the solar corona and inner heliosphere. Thanks to theuniqueness of Parker Solar Probe's (PSP) orbit, WISPR is able to image``locally'' coronal structures at high spatial and time resolutions. Theobserved plane of sky, however, rapidly changes because of the PSP's highorbital speed. Therefore, the interpretation of the dynamics of the coronalstructures recorded by WISPR is not straightforward. A first study, undertakenby \citet{Liewer2019}, shows how different coronal features (e.g., streamers,flux ropes) appear in the field of view of WISPR by means of raytracingsimulations. In particular, they analyze the effects of the spatial resolutionchanges on both the images and the associated height-time maps, and introducethe fundamentals for geometric triangulation. In this follow-up paper, we focuson the study of the total brightness of a simple, spherical, plasma densitystructure, to understand how the analysis of Thomson-scattered emission by theelectrons in a coronal feature can shed light into the determination of itskinematic properties. We investigate two cases: {\it (a)} a density sphere at aconstant distance from the Sun for different heliographic longitudes; {\it (b)}a density sphere moving outwardly with constant speed. The study allows us tocharacterize the effects of the varying heliocentric distance of the observerand scattering angle on the total brightness observed, which we exploit tocontribute to a better determination of the position and speed of the coronalfeatures observed by WISPR.

Simulating White-Light Images of Coronal Structures for Parker Solar Probe/WISPR: Study of the Total Brightness Profiles