We explore the origin of FUSE and HST STIS far UV spectra of the dwarf nova , EY Cyg , during its quiescence using combined high gravity photosphere and accretion disk models as well as model accretion belts .
The best-fitting single temperature white dwarf model to the FUSE plus HST STIS spectrum of EY Cygni has T _ { eff } = 24 , 000 K , log g = 9.0 , with an Si abundance of 0.1 x solar and C abundance of 0.2 x solar but the distance is only 301 pc .
The best-fitting composite model consists of white dwarf with T _ { eff } = 22 , 000 K , log g = 9 , plus an accretion belt with T _ { belt } = 36 , 000 K covering 27 % of the white dwarf surface with V _ { belt } sini = 2000 km/s .
The accretion belt contributes 63 % of the FUV light and the cooler white dwarf latitudes contribute 37 % .
This fit yields a distance of 351 pc which is within 100 pc of our adopted distance of 450 pc .
EY Cyg has very weak C iv emission and very strong N v emission , which is atypical of the majority of dwarf novae in quiescence .
We also conducted a morphological study of the surroundings of EY Cyg using direct imaging in narrow nebular filters from ground-based telescopes .
We report the possible detection of nebular material associated with EY Cygni .
Possible origins of the apparently large N v /C iv emission ratio are discussed in the context of nova explosions , contamination of the secondary star and accretion of nova abundance-enriched matter back to the white dwarf via the accretion disk or as a descendant of a precursor binary that survived thermal timescale mass transfer .
The scenario involving pollution of the secondary by past novae may be supported by the possible presence of a nova remnant-like nebula around EY Cyg .