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RS Oph is a recurrent symbiotic nova that undergoes nova-like outbursts on atime scale of 20 years. Its two last eruptions (1985 and 2006) were subject ofintensive multiwavelengths observational campaign from the X-rays to the radio.This contribution aims to determine physical parameters and the ionizationstructure of the nova from its explosion to the first emergence of thesupersoft X-rays (day 26) by using the method of multiwavelength modelling theSED. From the very beginning of the eruption, the model SED revealed thepresence of both a strong stellar and nebular component of radiation in thespectrum. During the first 4 days, the nova evinced a biconical ionizationstructure. The $\sim 8200$ K warm and 160 - 200 R$_{\odot}$ extendedpseudo-photosphere encompassed the white dwarf (WD) around its equator to thelatitude $>40^{\circ}$. The remaining space around the WD's poles was ionized,producing a strong nebular continuum with the emission measure $EM \sim 2.3\times 10^{62}$ cm$^{-3}$ via the fast wind from the WD. The luminosity of theburning WD was highly super-Eddington for the whole investigated period. Thewind mass loss at rates of $10^{-4} - 10^{-5}$ M$_{\odot}$yr$^{-1}$ and thepresence of jets suggest an accretion throughout a disk at a high rate, whichcan help to sustain the super-Eddington luminosity of the accretor for a longtime.

Multiwavelength modelling the SED of supersoft X-ray sources. II. RS Ophiuchi: From the explosion to the SSS phase