Modeling CHANDRA low energy transmission grating spectrometer observations of classical novae with PHOENIX I. V4743 Sagittarii

A. Petz, P. H. Hauschildt, J. U. Ness, Sumner Starrfield

Research output: Contribution to journalArticle

26 Citations (Scopus)

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 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.

Original languageEnglish (US)
Pages (from-to)321-328
Number of pages8
JournalAstronomy and Astrophysics
Volume431
Issue number1
DOIs
StatePublished - Feb 2005

Fingerprint

novae
spectrometer
gratings
spectrometers
modeling
energy
x rays
atmospheres
atmosphere
ejecta
thermodynamic equilibrium
bremsstrahlung
envelopes
thermodynamics
wavelength
wavelengths
temperature
code

Keywords

  • Atomic data
  • Stars: atmospheres
  • Stars: novae, cataclysmic variables
  • X-rays: individuals: V4743 Sgr

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Modeling CHANDRA low energy transmission grating spectrometer observations of classical novae with PHOENIX I. V4743 Sagittarii. / Petz, A.; Hauschildt, P. H.; Ness, J. U.; Starrfield, Sumner.

In: Astronomy and Astrophysics, Vol. 431, No. 1, 02.2005, p. 321-328.

Research output: Contribution to journalArticle

@article{54278f617da4460e845de0d73eff0309,
title = "Modeling CHANDRA low energy transmission grating spectrometer observations of classical novae with PHOENIX I. V4743 Sagittarii",
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 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.",
keywords = "Atomic data, Stars: atmospheres, Stars: novae, cataclysmic variables, X-rays: individuals: V4743 Sgr",
author = "A. Petz and Hauschildt, {P. H.} and Ness, {J. U.} and Sumner Starrfield",
year = "2005",
month = "2",
doi = "10.1051/0004-6361:20041396",
language = "English (US)",
volume = "431",
pages = "321--328",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",
number = "1",

}

TY - JOUR

T1 - Modeling CHANDRA low energy transmission grating spectrometer observations of classical novae with PHOENIX I. V4743 Sagittarii

AU - Petz, A.

AU - Hauschildt, P. H.

AU - Ness, J. U.

AU - Starrfield, Sumner

PY - 2005/2

Y1 - 2005/2

N2 - 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.

AB - 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.

KW - Atomic data

KW - Stars: atmospheres

KW - Stars: novae, cataclysmic variables

KW - X-rays: individuals: V4743 Sgr

UR - http://www.scopus.com/inward/record.url?scp=13844254265&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=13844254265&partnerID=8YFLogxK

U2 - 10.1051/0004-6361:20041396

DO - 10.1051/0004-6361:20041396

M3 - Article

VL - 431

SP - 321

EP - 328

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

IS - 1

ER -