Current best-known Drake Equation values? Frank Drake's equation is used to estimate $N$ the number of civilizations we might be able to communicate with in our galaxy:
$$N = R_\star f_p n_e f_l f_i f_c L$$
where:
$R_\star$ is the average rate of star formation in the galaxy
$f_p$ is the fraction of stars with planets
$n_e$ is the average number of goldilocks planets per planetary system
$f_l$ is the fraction of goldilocks planets that actually develop life
$f_i$ is the fraction of life bearing planets that develop intelligent life
$f_c$ is the fraction of civilizations that broadcast their existence into space
and $L$ is the length of time for which a civilization broadcasts their existence
Question
Have the many exoplanets we've discovered in the last several decades improved our estimates of $f_p$, and $n_e$?  Are these values different than what was guessed about prior to the discovery of the first exoplanets?  What is our current best estimate for $R_\star$ for the Milky Way?
Have the many exoplanets we've discovered in the last several decades improved our estimates of , and ?

Absolutely! The quantity $f_p n_e$ is a quantity of much interest in investigations of extrasolar planets, which effectively equates to the fraction of stars that have a habitable planet in their star's habitable zone. Plenty of studies have examined this specifically for Earth-sized extrasolar planets and place the value of $f_p n_e$ between ~$\frac{1}{6}$ (i.e. one in six stars have an earth-sized planet in a relatively close orbit to the host star) and ~$\frac{2}{5}$ [1][2]. A 2013 comprehensive study by Petigura is a great paper to get familiar with the specifics and assumptions of how the Kepler surveys are conducted and the quantities of interest calculated [3].

What is our current best estimate for ⋆ for the Milky Way?

Unfortunately the answer is: it varies. Roughly, we think that the Milky Way puts out about 3 solar masses worth of new star every year [4]. However, these don't have to be in one star. Since we think most stars are probably ~1 M$_\odot$, this works out to ~3 stars/year. However, some estimates go less, and some estimates (based on chemical decay of elements like aluminum) go as high as 7 stars/year [5].