  Extreme ultraviolet (EUV) coronal dimmings are often observed in response to
solar eruptive events. These phenomena can be generated via several different
physical processes. For space weather, the most important of these is the
temporary void left behind by a coronal mass ejection (CME). Massive, fast CMEs
tend to leave behind a darker void that also usually corresponds to minimum
irradiance for the cooler coronal emissions. If the dimming is associated with
a solar flare, as is often the case, the flare component of the irradiance
light curve in the cooler coronal emission can be isolated and removed using
simultaneous measurements of warmer coronal lines. We apply this technique to
37 dimming events identified during two separate two-week periods in 2011, plus
an event on 2010 August 7 analyzed in a previous paper, to parameterize dimming
in terms of depth and slope. We provide statistics on which combination of
wavelengths worked best for the flare-removal method, describe the fitting
methods applied to the dimming light curves, and compare the dimming parameters
with corresponding CME parameters of mass and speed. The best linear
relationships found are
  $$ \begin{align} v_{CME} \Big[\frac{km}{s} \Big] & \approx 2.36 \times 10^6
\Big[\frac{km}{\%} \Big] \times s_{dim} \Big[\frac{\%}{s} \Big] \\ m_{CME} [g]
& \approx 2.59 \times 10^{15} \Big[\frac{g}{\%} \Big] \times \sqrt{d_{dim}}
[\%]. \end{align} $$
  These relationships could be used for space weather operations of estimating
CME mass and speed using near-realtime irradiance dimming measurements.
