We have fitted the Chandra Low Energy Transmission Grating spectrum of SS Cygni in outburst with a single temperature blackbody suffering the photoelectric opacity of a neutral column density and the scattering opacity of an outflowing wind .
We find that this simple model is capable of reproducing the essential features of the observed spectrum with the blackbody temperature T _ { bl } \approx 250 \pm 50 kK , hydrogen column density N _ { H } \approx 5.0 ^ { +2.9 } _ { -1.5 } \times 10 ^ { 19 } ~ { } cm ^ { -2 } , fractional emitting area f \approx 5.6 ^ { +60 } _ { -4.5 } \times 10 ^ { -3 } , boundary layer luminosity L _ { bl } \approx 5 ^ { +18 } _ { -3 } \times 10 ^ { 33 } ~ { } erg~ { } s ^ { -1 } , wind velocity v \approx 2500 ~ { } km~ { } s ^ { -1 } , wind mass-loss rate \dot { M } _ { w } \approx 1.1 \times 10 ^ { 16 } ~ { } g~ { } s ^ { -1 } , and arbitrary values of the wind ionization fractions of 20 ions of O , Ne , Mg , Si , S , and Fe .
Given that in outburst the accretion disk luminosity L _ { disk } \approx 1 \times 10 ^ { 35 } ~ { } erg~ { } s ^ { -1 } , L _ { bl } / L _ { disk } \approx 0.05 ^ { +0.18 } _ { -0.03 } , which can be explained if the white dwarf ( or an equatorial belt thereon ) is rotating with an angular velocity \Omega _ { wd } \approx 0.7 ^ { +0.1 } _ { -0.2 } 
Hz , hence V _ { rot } \sin i \sim 2300 ~ { } km~ { } s ^ { -1 } .