  Filament eruptions often lead to coronal mass ejections (CMEs) on the Sun and
are one of the most energetic eruptive phenomena in the atmospheres of other
late-type stars. However, the detection of filament eruptions and CMEs on stars
beyond the solar system is challenging. Here we present six filament eruption
cases on the Sun and show that filament material obscuring part of the solar
disk can cause detectable dimming signatures in sun-as-a-star flux curves of He
II 304 A. Those filament eruptions have similar morphological features,
originating from small filaments inside active regions and subsequently
strongly expanding to obscure large areas of the solar disk or the bright flare
regions. We have tracked the detailed evolution of six obscuration dimmings and
estimated the dimming properties, such as dimming depths, dimming areas, and
duration. The largest dimming depth among the six events under study is 6.2%
accompanied by the largest dimming area of 5.6\% of the solar disk area. Other
events have maximum dimming depths in a range of around 1% to 3% with maximum
areas varying between about 3% to 4% of the solar disk area. The duration of
the dimming spans from around 0.4 hours to 7.0 hours for the six events under
study. A positive correlation was found between the dimming depth and area,
which may help to set constraint on the filament sizes in stellar observations.
