XMM-Newton X-ray and ultraviolet observations of the fast nova V2491Cyg during the supersoft source phase

J. U. Ness, J. P. Osborne, A. Dobrotka, K. L. Page, J. J. Drake, C. Pinto, R. G. Detmers, G. Schwarz, M. F. Bode, A. P. Beardmore, Sumner Starrfield, M. Hernanz, G. Sala, J. Krautter, C. E. Woodward

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Abstract

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, during the supersoft source (SSS) phase, yielding simultaneous X-ray and UV light curves and high-resolution X-ray spectra. The first X-ray light curve is highly variable, showing oscillations with a period of 37.2minutes after an extended factor of three decline lasting ∼3 hr, while the second X-ray light curve is less variable. The cause of the dip is currently unexplained and has most likely the same origin as similar events in the early SSS light curves of the novae V4743Sgr and RSOph, as it occurred on the same timescale. The oscillations are not present during the dip minimum and also not in the second observation. The UV light curves are variable but contain no dips and no period. High-resolution X-ray spectra are presented for four intervals of differing intensity. All spectra are atmospheric continua with deep absorption lines and absorption edges. Two interstellar lines of O I and N I are clearly seen at their rest wavelengths, while a large number of high-ionization absorption lines are found at blueshifts indicating an expansion velocity of 3000-3400kms -1, which does not change significantly during the epochs of observation. Comparisons with the slower nova V4743Sgr and the symbiotic recurrent nova RSOph are presented. The SSS spectrum of V4743Sgr is much softer with broader and more complex photospheric absorption lines. The ejecta are extended, allowing us to view a larger range of the radial velocity profile. Meanwhile, the absorption lines in RSOph are as narrow as in V2491Cyg, but they are less blueshifted. A remarkable similarity in the continua of V2491Cyg and RSOph is found. The only differences are smaller line shifts and additional emission lines in RSOph that are related to the presence of a dense stellar wind from the evolved companion. Three unidentified absorption lines are present in the X-ray spectra of all three novae, with projected rest wavelengths 26.05 Å, 29.45 Å, and 30.0 Å. No entirely satisfactory spectral model is currently available for the soft X-ray spectra of novae in outburst, and careful discussion of assumptions is required.

Original languageEnglish (US)
Article number70
JournalAstrophysical Journal
Volume733
Issue number1
DOIs
StatePublished - May 20 2011

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Keywords

  • astronomical databases: miscellaneous
  • novae, cataclysmic variables
  • stars: individual (V2491 Cyg, RS Oph, V4743 Sgr)

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Ness, J. U., Osborne, J. P., Dobrotka, A., Page, K. L., Drake, J. J., Pinto, C., Detmers, R. G., Schwarz, G., Bode, M. F., Beardmore, A. P., Starrfield, S., Hernanz, M., Sala, G., Krautter, J., & Woodward, C. E. (2011). XMM-Newton X-ray and ultraviolet observations of the fast nova V2491Cyg during the supersoft source phase. Astrophysical Journal, 733(1), [70]. https://doi.org/10.1088/0004-637X/733/1/70