A&A 431, 321-328 (2005)
DOI: 10.1051/0004-6361:20041396
Modeling CHANDRA low energy transmission grating spectrometer observations of classical novae with PHOENIX
I. V4743 Sagittarii
A. Petz1, P. H. Hauschildt1, J.-U. Ness1 and S. Starrfield21 Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany
e-mail: [apetz;yeti;jness]@hs.uni-hamburg.de
2 Department of Physics and Astronomy, Arizona State University, Tempe, AZ 58287-1504, USA
e-mail: starrfield@asu.edu
(Received 3 June 2004 / Accepted 1 October 2004 )
Abstract
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 1D 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
=
5.8
105 K, with
= 50 000
. The models are calculated for solar
abundances. It is shown that the models can be used to determine
abundances in the nova ejecta.
Key words: stars: novae, cataclysmic variables -- X-rays: individuals: V4743 Sgr -- stars: atmospheres -- atomic data
SIMBAD Objects
© ESO 2005

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