The Properties of X-Ray and Optical Light Curves of X-Ray Novae

Details The Properties of X-Ray and Optical Light Curves of X-Ray Novae The Properties of X-Ray and Optical Light Curves of X-Ray Novae

1997-07-11

arxiv.org/abs/astro-ph/9707138v1

Astrophys.J. 491 (1997) 312

Astronomy and Astrophysics

Astrophysics

68 pages including 27 Postscript figures and 12 tables. To be published in the Astrophysical Journal, Part 1

Scientific paper

10.1086/304921

We have collected the available data from the literature and from public data archives covering the past two decades for the long-term X-ray and optical light curves of X-ray nova (XN) outbursts, and carry out for the first time a systematic, statistical study of XN light curves which are classified into 5 morphological types. Basic light curve parameters, e.g., the outburst peak flux, amplitude, luminosity, rise and decay timescales, the observed and expected outburst durations, and total energy radiated, are tabulated and discussed. The rise timescales are found to have a flat distribution while the decay timescales have a much narrower and near-Gaussian distribution, centered around 30 days and dominated by the strongest outbursts. The peak luminosity is also distributed like a Gaussian, centered around 0.2 in Eddington units, while the total energy released has a much broader distribution around 10E44 ergs. We identify and discuss additional light curve features, such as precursors, plateaus, and secondary maxima. The plateaus exhibited in the light curves of black hole sources are found to have, on average, longer durations and they are followed by longer decays. The identified secondary maxima seem to occur mostly in black hole systems. For the frequency of outbursts, we find that the average XN outburst rate is about 2.6 per year for events >0.3 Crab, and that the mean recurrence time between outbursts from a single source is 6 years. The spatial and logN-logS distribution of the XN sources, with limited statistics, agrees with a source population in the Galactic disk, as observed from a point at a distance of 8.5 kpc from the Galactic center. Finally, we point out that the observed XN light curve properties can in general be explained by a disk thermal instability model, although some important problems still remain.

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