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The variable iron line in cygnus X-3

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Abstract

Cygnus X-3 was observed with the GSPC on board EXOSAT on several occasions, one observation lasting for 7 orbital cycles. The width W and centroid energy E of the iron emission feature near 6.7 keV show a smooth, correlated, sinusoidal-type modulation, the iron line being widest and E being lowest just before X-ray maximum. The line profile may show a low-energy wing, but apart from this does not deviate strongly from a symmetric, Gaussian-type shape. The continuum at higher energies than the line is not completely smooth, but shows ‘bumps’ which remain stable in time. Two possible explanations are discussed for the correlated variation of E and W as a function of orbital phase.

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Authors and Affiliations

  1. Space Science Department of ESA, ESTEC, Postbus 299, 2200AG, Noordwijk, The Netherlands

    A. Smith

  2. EXOSAT Observatory, ESOC, Robert-Bosch-Strasse 5, 61, Darmstadt, West Germany

    N. White

  3. Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey, England

    K. Mason

  4. IFCI/CNR, Via M. Stabile 172, 90139, Palermo, Italy

    G. Manzo

Authors
  1. M. van der Klis
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  2. A. Peacock
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  3. A. Smith
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  4. N. White
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  5. K. Mason
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  6. G. Manzo
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van der Klis, M., Peacock, A., Smith, A. et al. The variable iron line in cygnus X-3. Space Sci Rev 40, 297–304 (1985). https://doi.org/10.1007/BF00212902

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  • DOI: https://doi.org/10.1007/BF00212902

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