Variability of accretion flow in the core of the Seyfert galaxy NGC 4151

Details Variability of accretion flow in the core of the Seyfert galaxy NGC 4151 Variability of accretion flow in the core of the Seyfert galaxy NGC 4151

2001-10-31

arxiv.org/abs/astro-ph/0110708v2

Mon.Not.Roy.Astron.Soc. 342 (2003) 1222

Astronomy and Astrophysics

Astrophysics

21 pages, 19 figures, 4 tables, accepted for publication in MNRAS

Scientific paper

10.1046/j.1365-8711.2003.06623.x

We analyze observations of the Seyfert galaxy NGC 4151 covering 90 years in the optical band and 27 years in the 2-10 keV X-ray band. We compute the Normalized Power Spectrum Density (NPSD), the Structure Function (SF) and the Autocorrelation Function (ACF) for these data. The results show that the optical and X-ray variability properties are significantly different. X-ray variations are predominantly in the timescale range of 5 - 1000 days. The optical variations have also a short timescale component which may be related to X-ray variability but the dominant effect is the long timescale variability, with timescales longer than $\sim$ 10 years. We compare our results with observations of NGC 5548 and Cyg X-1. We conclude that the long timescale variability may be caused by radiation pressure instability in the accretion disk, although the observed timescale in NGC 4151 is by a factor of few longer than expected. X-ray variability of this source is very similar to what is observed in Cyg X-1 but scaled with the mass of the black hole, which suggests that the radiation pressure instability does not affect considerably the X-ray production.

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