Constraining accretion from coordinated multi-wavelength rapid timing observations of X-ray binaries

Details Constraining accretion from coordinated multi-wavelength rapid timing observations of X-ray binaries Constraining accretion from coordinated multi-wavelength rapid timing observations of X-ray binaries

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010fym..confe...8g&link_type=abstract

"The First Year of MAXI: Monitoring Variable X-ray Sources", 4th International MAXI Workshop held November 30 - December 2, 2010

Physics

Scientific paper

It has long been believed that the optical and infrared (OIR) fluxes of compact accreting sources will not generally show fast, stochastic variability. This is because reprocessing of high energy photons is thought to be the primer driver of the OIR fluxes. In recent work, we have found fast (sub-second) optical variations in accreting black hole and neutron star binaries. The power spectra of the source light curves show wide-band noise and even low-frequency quasi-periodic oscillations. These are characteristics very similar to those found in X-ray observations. The OIR fluxes show some clear and intriguing correlations with the X-ray fluxes on timescales of 0.1-10 s, which can place quantitative physical constraints on the accretion processes for the first time. Detailed statistical analyses including the inter-band coherence, phase lags and rms spectrum will be discussed. These show unambiguously that at least two separate components (e.g. a jet and a corona) are interacting via some underlying connections (e.g. a strong magnetic field threading the entire inner flow regions). OIR timing studies are thus proving detailed insight on compact accreting sources, complementing X-ray constraints.

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