  We present the second part (days 19 to 102) of our high-resolution Echelle
atlas of the spectral evolution of RS Oph during the 2021 nova outburst. Some
quick conclusions that can be drawn are: (1) the spectra evolution has
progressed smoothly, suggesting that both the expansion of the ejecta through
the pre-existing RG wind and the photo-ionization from the central source did
not encountered sudden discontinuities prior to switch-off of the nuclear
burning; (2) the 2021 spectral evolution is similar to that of the 2006
eruption, with a mirror-appearance of the triple-peaked line profiles (blue
peak brighter than red in 2006, the opposite in 2021); (3) the evolution of the
triple-peaked profiles progressed similarly through different excitation and
ionization degrees, suggesting an origin in a bipolar outflow nested to an
equatorial torus; (4) the time-behavior of coronal emission lines appears quite
smooth, both in terms of radiated flux as well as evolution of the
triple-peaked profiles, with a plateau at maximum lasting up to about day 87;
(5) there seems to exist within RS Oph two distinct types of ejecta: one fast
moving and producing Gaussian-like line profiles (primarely [NII] and [OIII]),
that keep expanding at FWHM=1000 km/s with no sign of ongoing deceleration
during the two months leading up to Solar conjunction, and slower moving ejecta
giving rise to the triple-peaked line profiles (HeI, HeII, coronal lines, and
also Balmer lines at later times), for which the separation in velocity of blue
and red peaks is still shrinking at the time of Solar conjunction when it
reaches an average of 330 km/s; (6) the "symbiotic band" at 6825 Ang, due to
Raman scattering of OVI 1032 by neutral hydrogen, appears simultaneously with
the coronal lines: its very presence indicates that a sizeable part of the wind
of the red giant has remained neutral during the development of coronal lines.
