The solar corona and chromosphere are often marked by eruptive features, such as flares, prominences, loops, and coronal mass ejections, which rise above the photospheric surface. Coronal streamers and plumes can also characterize the outer atmosphere of the Sun. All of these structures, fascinating in their extent and formation, frequently emit continuous spectra and can usually be observed using white-light coronagraphs. This implies, at least in part, that they are comprised of condensed matter. The continuous spectra associated with chromospheric and coronal structures can be viewed as representing the twenty-eighth line of evidence, and the eighth Planckian proof, that the Sun is condensed matter. The existence of such objects also suggests that the density of the solar atmosphere rises to levels well in excess of current estimates put forth by the gaseous models of the Sun. In this work, the densities of planetary atmospheres are examined in order to gain insight relative to the likely densities of the solar chromosphere. Elevated densities in the solar atmosphere are also supported by coronal seismology studies, which can be viewed as constituting the twenty-ninth line of evidence that the Sun is composed of condensed matter.