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