Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008mnras.388..921p&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 388, Issue 2, pp. 921-926.
Astronomy and Astrophysics
Astronomy
3
Binaries: Close, Stars: Individual: Rr Pic, Novae, Cataclysmic Variables, Stars: Rotation, White Dwarfs, X-Rays: Stars
Scientific paper
We present the Chandra ACIS-S3 data of the old classical nova RR Pic (1925). The source has a count rate of 0.067 +/- 0.002 count s-1 in the 0.3-5.0 keV energy range. We detect the orbital period of the underlying binary system in the X-ray wavelengths. We also find that the neutral hydrogen column density differs for orbital minimum and orbital maximum spectra with values 0.25+0.23-0.18 × 1022 and 0.64+0.13-0.14 × 1022cm-2 at 3σ confidence level. The X-ray spectrum of RR Pic can be represented by a composite model of bremsstrahlung with a photoelectric absorption, two absorption lines centered around 1.1-1.4 keV and five Gaussian lines centered at emission lines around 0.3-1.1 keV corresponding to various transitions of S, N, O, C, Ne and Fe. The bremsstrahlung temperature derived from the fits ranges from 0.99 to 1.60 keV and the unabsorbed X-ray flux is found to be 2.5+0.4-1.2 × 10-13ergcm-2s-1 in the 0.3-5.0 keV range with a luminosity of 1.1 +/- 0.2 1031ergs-1 at 600 pc. We also detect excess emission in the spectrum possibly originating from the reverse shock in the ejecta. A fit with a cooling flow plasma emission model shows enhanced abundances of He, C, N, O and Ne in the X-ray emitting region indicating existence of diffusive mixing.
Balman Soelen
Pekon Yakup
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