NLTE model atmospheres for the hottest white dwarfs: Spectral analysis of the compact component in nova V4743 Sgr
Thomas Rauch,Marina Orio,R. Gonzales-Riestra,T. J. N. Nelson,Martin Still,K. Werner,Jörn Wilms +6 more
TL;DR: In this paper, a grid of synthetic energy distributions (SEDs) based on NLTE model atmospheres was calculated for the analysis of the hottest white dwarfs and present the result of fits to Chandra and XMM-Newton grating X-ray spectra of V4743 Sgr of outstanding quality.
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Abstract: Half a year after its outburst in September 2002, nova V4743 Sgr evolved into the brightest supersoft X-ray source in the sky with a flux maximum around 30A. We calculated grids of synthetic energy distributions (SEDs) based on NLTE model atmospheres for the analysis of the hottest white dwarfs and present the result of fits to Chandra and XMM-Newton grating X-ray spectra of V4743 Sgr of outstanding quality, exhibiting prominent resonance lines of C V, C VI, N VI, N VII, and O VII in absorption. The nova reached its highest effective temperature (Teff = 740 +/- 70kK) around April 2003 and remained at that temperature at least until September 2003. We conclude that the white dwarf is massive, about 1.1 - 1.2 Msun. The nuclear-burning phase lasted for 2 to 2.5 years after the outburst, probably the average duration for a classical nova. The photosphere of V4743 Sgr was strongly carbon deficient (about times solar) and enriched in nitrogen and oxygen (> 5 times solar). Especially the very low C/N ratio indicates that the material at the white dwarf's surface underwent thermonuclear burning. Thus, this nova retained some of the accreted material and did not eject all of it in outburst. From March to September 2003, the nitrogen abundance is strongly decreasing, probably new material is already been accreted at this stage.
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Hydrogen Burning on Accreting White Dwarfs: Stability, Recurrent Novae, and the Post-nova Supersoft Phase
TL;DR: In this paper, the authors examined the properties of white dwarfs (WDs) accreting hydrogen-rich matter in and near the stable burning regime of accretion rates as modeled by time-dependent calculations done with Modules for Experiments in Stellar Astrophysics.
255
Swift X-Ray Observations of Classical Novae. II. The Super Soft Source Sample
Greg J. Schwarz,Jan-Uwe Ness,J. P. Osborne,K. L. Page,Phil Evans,A. P. Beardmore,Frederick M. Walter,L. Andrew Helton,Charles E. Woodward,M. F. Bode,Sumner Starrfield,Jeremy J. Drake +11 more
- 29 Nov 2011
TL;DR: Swift observations of 52 Galactic/Magellanic Cloud novae are presented indicating that additional factors beyond the white dwarf mass and binary separation play important roles in the evolution of a nova outburst and two optical phenomena are confirmed that are correlated with strong, soft X-ray emission which can be used to further increase the efficiency ofX-ray campaigns.
Hydrogen Burning on Accreting White Dwarfs: Stability, Recurrent Novae, and the Post-Novae Supersoft Source
TL;DR: In this paper, the authors examined the properties of white dwarfs (WDs) accreting hydrogen-rich matter in and near the stable burning regime of accretion rates as modeled by time-dependent calculations done with Modules for Experiments in Stellar Astrophysics (MESA).
161
The supersoft x-ray phase of nova rs ophiuchi 2006
J. P. Osborne,K. L. Page,A. P. Beardmore,M. F. Bode,M. R. Goad,Tim O'Brien,Sumner Starrfield,Thomas Rauch,Jan-Uwe Ness,Joachim Krautter,Greg J. Schwarz,David N. Burrows,N. Gehrels,J. J. Drake,A. Evans,S. P. S. Eyres +15 more
TL;DR: Measurements are consistent with a WD mass near the Chandrasekhar limit; combined with a deduced accumulation of mass transferred from its binary companion, this leads to suggest that RS Oph is a strong candidate for a future supernova explosion.
136
XMM-NEWTON X-RAY AND ULTRAVIOLET OBSERVATIONS OF THE FAST NOVA V2491 Cyg DURING THE SUPERSOFT SOURCE PHASE
Jan-Uwe Ness,J. P. Osborne,A. Dobrotka,K. L. Page,J. J. Drake,Ciro Pinto,R. G. Detmers,Greg J. Schwarz,M. F. Bode,A. P. Beardmore,Sumner Starrfield,M. Hernanz,Gloria Sala,Joachim Krautter,Charles E. Woodward +14 more
TL;DR: Two XMM-Newton observations of the fast classical nova V2491Cyg were carried out in short succession on days 39.93 and 49.62 after discovery, yielding simultaneous X-ray and UV light curves and high-resolution X-rays spectra, finding a remarkable similarity in the continua of V24 91Cyg and RSOph.
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