The spectroscopic characteristics of great auroras during two superstorms of February 8–9, 1986, and March 13–14, 1989, are compared. The first storm occurred during the intensity minimum of solar activity, whilst the second one occurred at the time maximum activity phase of solar cycle 22. The storm of February 8–9, 1986, (min Dst = −312 nT) was produced by plasma fluxes generated by a series of
... [Show full abstract] solar flares of minor intensity, whereas the second storm on March 13–14, 1989, (min Dst = −600 nT) resulted from particle fluxes from an intense solar flare and exceptionally bright coronal mass ejection (CME). During these two superstorms there were great auroras observed, which were fundamentally different in their spectroscopic characteristics. In the first case, (Loparskaya obs.) intense green IBC 3 aurora were observed during the whole night in the auroral zone. The intensity of the green oxygen line λ 557.7 nm [0I] was > 100 kR, and the ratio of the emission intensity was . In the second case (March 13–14, 1989), intense type A red auroras were observed. In the auroral zone (Loparskaya obs.), the intensity of the red oxygen line λ 630.0 nm [0I] reached 300 kR, whereas the ratio of emission intensity during the whole night. Such a difference in the spectral characteristics of the auroras may be determined either by different energetic spectra of the precipitating particles, or by different properties of the upper atmosphere during the years of low and high solar acivity.