Context : In 1996 , Sakurai ’ s object ( V4334 Sgr ) suddenly brightened in the centre of a faint Planetary Nebula ( PN ) .
This very rare event was interpreted as the reignition of a hot white dwarf that caused a rapid evolution back to the cool giant phase .
From 1998 on , a copious amount of dust has formed continuously , screening out the star which has remained embedded in this expanding high optical depth envelope .

Aims : The new observations , reported here , are used to study the morphology of the circumstellar dust in order to investigate the hypothesis that Sakurai ’ s Object is surrounded by a thick spherical envelope of dust .

Methods : We have obtained unprecedented , high-angular resolution spectro-interferometric observations , taken with the mid-IR interferometer MIDI/VLTI , which resolve the dust envelope of Sakurai ’ s object .

Results : We report the discovery of a unexpectedly compact ( 30 x 40 milliarcsec , 105 x 140 AU assuming a distance of 3.5 kpc ) , highly inclined , dust disk .
We used Monte Carlo radiative-transfer simulations of a stratified disk to constrain its geometric and physical parameters , although such a model is only a rough approximation of the rapidly evolving dust structure .
Even though the fits are not fully satisfactory , some useful and robust constraints can be inferred .
The disk inclination is estimated to be 75 ^ { \circ } \pm 3 ^ { \circ } with a large scale height of 47 \pm 7 AU .
The dust mass of the disk is estimated to be 6 \times 10 ^ { -5 } M _ { \odot } .
The major axis of the disk ( 132 ^ { \circ } \pm 3 ^ { \circ } ) is aligned with an asymmetry seen in the old PN that was re-investigated as part of this study .
This implies that the mechanism responsible for shaping the dust envelope surrounding Sakurai ’ s object was already at work when the old PN formed .

Conclusions :