We use the PHOENIX code package to model the X-ray spectrum of Nova V4743 Sagittarii observed with the LETGS onboard the Chandra satellite 19 March 2003. Our atmosphere models are ID spherical, expanding, line blanketed, and in full non-local thermodynamic equilibrium. To analyze nova atmospheres and related systems with an underlying nuclear burning envelope at X-ray wavelengths, it was necessary to update the code with new microphysics, as discussed in this paper. We demonstrate that the X-ray emission is dominated by thermal bremsstrahlung and that the hard X-rays are dominated by Fe and N absorption. The best fit to the observation is provided at a temperature of Teff = 5.8 × 105 K, with Lbol = 50000 L⊙. The models are calculated for solar abundances. It is shown that the models can be used to determine abundances in the nova ejecta.
- Atomic data
- Stars: atmospheres
- Stars: novae, cataclysmic variables
- X-rays: individuals: V4743 Sgr
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science