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We present the second part (days 19 to 102) of our high-resolution Echelleatlas of the spectral evolution of RS Oph during the 2021 nova outburst. Somequick conclusions that can be drawn are: (1) the spectra evolution hasprogressed smoothly, suggesting that both the expansion of the ejecta throughthe pre-existing RG wind and the photo-ionization from the central source didnot encountered sudden discontinuities prior to switch-off of the nuclearburning; (2) the 2021 spectral evolution is similar to that of the 2006eruption, with a mirror-appearance of the triple-peaked line profiles (bluepeak brighter than red in 2006, the opposite in 2021); (3) the evolution of thetriple-peaked profiles progressed similarly through different excitation andionization degrees, suggesting an origin in a bipolar outflow nested to anequatorial torus; (4) the time-behavior of coronal emission lines appears quitesmooth, both in terms of radiated flux as well as evolution of thetriple-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 fastmoving and producing Gaussian-like line profiles (primarely [NII] and [OIII]),that keep expanding at FWHM=1000 km/s with no sign of ongoing decelerationduring the two months leading up to Solar conjunction, and slower moving ejectagiving rise to the triple-peaked line profiles (HeI, HeII, coronal lines, andalso Balmer lines at later times), for which the separation in velocity of blueand red peaks is still shrinking at the time of Solar conjunction when itreaches an average of 330 km/s; (6) the "symbiotic band" at 6825 Ang, due toRaman scattering of OVI 1032 by neutral hydrogen, appears simultaneously withthe coronal lines: its very presence indicates that a sizeable part of the windof the red giant has remained neutral during the development of coronal lines.

The 2021 outburst of RS Oph: a pictorial atlas of the spectroscopic evolution. II. From day 19 to 102 (solar conjunction)