  In this paper we estimate the "star formation change parameter", SFR$_{79}$,
which characterizes the current SFR relative to the average during the last 800
Myr, for $\sim$ 300'000 galaxies selected from the Sloan Digital Sky Survey
(SDSS). The goals are to examine, in a much larger and independent sample, the
trends previously reported in a sample of star-forming MaNGA galaxies, and also
to search for spectroscopic signatures of ongoing quenching in the so-called
"Green Valley", which is generally believed to contain galaxies that are
migrating from the star-forming (SF) population to the quenched population of
galaxies. Measuring SFR$_{79}$ for our large sample of SDSS galaxies, we first
confirm the basic results of SF galaxies published by Wang & Lilly. We then
discuss in detail the calibration and meaning of SFR$_{79}$ for galaxies that
are well below the SFMS and establish the expected statistical signature of
systematic ongoing quenching from modelling the z$\sim$0 quenching rate of the
SF population. We conclude that it is not possible at present to establish
unambiguous observational evidence for systematic ongoing quenching processes,
due to limitations both in the noise of the observational data, in particular
in the measurements of H$\delta$ absorption, and in the calibration of
SFR$_{79}$, as well as biases introduced by the necessity of selecting objects
with significant H$\alpha$ emission. We do however see plausible indications of
ongoing quenching, which are quantitatively consistent with expectations from
"growth+quenching" models of galaxy evolution and a typical e-folding timescale
for quenching of $\sim500$ Myr.
