  In our previous articles (Chertok et al.: 2013, Solar Phys. 282, 175, and
2015, Solar Phys. 290, 627), we presented a preliminary tool for the early
diagnostics of the geoeffectiveness of solar eruptions based on the estimate of
the total unsigned line-of-sight photospheric magnetic flux in accompanying
extreme-ultraviolet arcades and dimmings. This tool was based on the analysis
of eruptions observed in 1996-2005 with SOHO/EIT and MDI. Empirical
relationships were obtained to estimate the probable importance of upcoming
space weather disturbances caused by an eruption, which just occurred, without
data on the associated coronal mass ejections. It was possible to estimate the
intensity of a non-recurrent geomagnetic storm (GMS) and Forbush decrease (FD),
as well as their onset and peak times. After 2010-2011, data on solar eruptions
are obtained with SDO/AIA and HMI. We use relatively short intervals of
overlapping EIT-AIA and MDI-HMI detailed observations and a number of large
eruptions over the next five years with the 12-hour cadence EIT images to adapt
the SOHO diagnostic tool to SDO data. The adopted brightness thresholds select
from the EIT 195 \AA\ and AIA 193 \AA\ image practically the same areas of
arcades and dimmings with a cross-calibration factor of 3.6-5.8 (5.0-8.2) for
the AIA exposure time of 2.0 s (2.9 s). For the same photospheric areas, the
MDI magnetic flux systematically exceeds the HMI flux by a factor of 1.4. Based
on these results, the empirical diagnostic relationships obtained from SOHO
data are adjusted to SDO instruments. Examples of a post-diagnostics based on
SDO data are presented. As before, the tool is applicable to non-recurrent GMSs
and FDs caused by nearly central eruptions from active regions, provided that
the southern component of the interplanetary magnetic field near the Earth is
predominantly negative, which is not predicted by this tool.
