Photometric observations of the radio bright B[e]/X-ray binary CI Cam

Details Photometric observations of the radio bright B[e]/X-ray binary CI Cam Photometric observations of the radio bright B[e]/X-ray binary CI Cam

Apr 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26a...356...50c&link_type=abstract

Astronomy and Astrophysics, v.356, p.50-62 (2000)

Astronomy and Astrophysics

Astrophysics

38

Stars: Binaries: General, Stars: Circumstellar Matter, Stars: Individual:, Stars: Winds, Outflows, X-Rays: Stars

Scientific paper

We present multiwavelength (optical, IR, radio) observations of CI Cam, the optical counterpart to the transient X-ray source XTE J0421+560. Pre-outburst quiescent observations reveal the presence of a dusty envelope around the system. Pronounced short term variability is observed at all wavebands from U-K, but no indication of prior flaring of a similar magnitude to the 1998 April outburst is found in these data. Data obtained during the 1998 April X-ray flare reveal pronounced optical-radio flaring. The optical flux was observed to quickly return to quiescent levels, while the radio flare was of much longer duration. The optical component is likely to result from a combination of free-free/free-bound emission, emission line and thermal dust emission, caused by re-radiation of the X-ray flux, while the behaviour of the multiwavelength radio data is consistent with emission from expanding ejecta emitting via the synchrotron mechanism. Post-outburst (1998 August-1999 March) U-M broadband photometric observations reveal that while the optical (UBV) flux remains at pre-outburst quiescent levels, near IR (JHKLM) fluxes exceed the pre-outburst fluxes by ~ 0.5 magnitudes. Modelling the pre- and post-outburst spectral energy distribution of CI Cam reveals that the structure and/or composition of the dusty component of the circumstellar envelope appears to have changed. Due to a lack of information on the precise chemical composition of the dust within the system several explanations for this behaviour are possible, such as the production of new dust at the inner edge of the envelope, or modification of the composition of the dust due to X-ray irradiation.

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