We report on the analysis of an X-ray grating spectrum of the Classical Nova V382 Vel ( 1999 ) , obtained with the LETG+HRC-S instrument on board CHANDRA , which shows emission lines dominating over any continuum .
Lines of Si , Mg , Ne , O , N , and C are identified , but no Fe lines are detected .
The total luminosity in the lines is \sim 4 \times 10 ^ { 27 } erg s ^ { -1 } ( corrected for N _ { H } = 1.2 \times 10 ^ { 21 } cm ^ { -2 } ) .
The lines have broad profiles with FWHM corresponding to a velocity \sim 2900 \pm 200 km s ^ { -1 } .
Some structure is identified in the profiles , but for different elements we find different profile structures .
While lines of O show a broadened Gaussian profile , those of Ne are double-peaked , suggesting a fragmented emitting plasma .
Using the emission measure distribution we derive relative element abundances and find abundances of Ne and N that are significantly enhanced relative to that of O , while Fe is not over-abundant .
The lack of any source emission longwards of 50 Å and the O viii Ly _ { \alpha } /Ly _ { \beta } line ratio support previous values of the hydrogen column-density .
We find weak continuum emission from the white dwarf , consistent with a black-body spectrum with an upper limit to the temperature of T = 3 \times 10 ^ { 5 } K , assuming a source radius of 6000 km .
The upper limit for the integrated black-body luminosity is 2 \times 10 ^ { 36 } erg s ^ { -1 } .
The BeppoSAX and Chandra ACIS observations of V382 Vel show that the nova was bright and in the Super Soft phase as late as 1999 December 30 .
Our LETG observation obtained 6 weeks later , as well as all subsequent X-ray observations , showed a remarkable fading to a nearly pure emission line phase which suggests that nuclear burning on the white dwarf had turned off by February .
In the absence of a photoionizing source the emission lines were formed in a collisionally ionized and excited expanding shell .