Journal Article

RR Pic (1925): a <i>Chandra</i> X-ray view

Y. Pekön and Ş. Balman

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 388, issue 2, pages 921-926
Published in print August 2008 | ISSN: 0035-8711
Published online July 2008 | e-ISSN: 1365-2966 | DOI:
RR Pic (1925): a Chandra X-ray view

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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× 10−13erg cm−2s−1 in the 0.3–5.0 keV range with a luminosity of 1.1 ± 0.2 1031erg s−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.

Keywords: binaries: close; stars: individual: RR Pic; novae, cataclysmic variables; stars: rotation; white dwarfs; X-rays: stars

Journal Article.  4003 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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