SAX J1808.4-3658 and the origin of X-ray variability in X-ray binaries and active galactic nuclei

Details SAX J1808.4-3658 and the origin of X-ray variability in X-ray binaries and active galactic nuclei SAX J1808.4-3658 and the origin of X-ray variability in X-ray binaries and active galactic nuclei

2003-11-19

arxiv.org/abs/astro-ph/0311453v1

Mon.Not.Roy.Astron.Soc. 347 (2004) L61

Astronomy and Astrophysics

Astrophysics

6 pages, 3 figures. Accepted for publication in MNRAS Letters

Scientific paper

10.1111/j.1365-2966.2004.07434.x

The aperiodic X-ray variability in neutron star and black hole X-ray binaries (XRBs), and active galactic nuclei (AGN) shows a characteristic linear relationship between rms amplitude and flux, implying a multiplying-together or `coupling' of variability on different time-scales. Such a coupling may result from avalanches of flares, due to magnetic reconnection in an X-ray emitting corona. Alternatively this coupling may arise directly from the coupling of perturbations in the accretion flow, which propagate to the inner emitting regions and so modulate the X-ray emission. Here, we demonstrate explicitly that the component of aperiodic variability which carries the rms-flux relation in the accreting millisecond pulsar SAX J1808.4-3658 is also coupled to the 401 Hz pulsation in this source. This result implies that the rms-flux relation in SAX J1808.4-3658 is produced in the accretion flow on to the magnetic caps of the neutron star, and not in a corona. By extension we infer that propagating perturbations in the accretion flow, and not coronal flares, are the source of the rms-flux relations and hence the aperiodic variability in other XRBs and AGN.

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