MG15 - Talk detail

Back to previous page

 Participant

Institution

Session

Accepted

Yes

Order

Time

Talk

Title

Abstract

MAXI J1836-194 is a black hole candidate X-ray binary, discovered during an outburst in 2011. It was observed at several different phases of the outburst with an excellent multi-wavelength coverage (Russell et al. 2013). In most of these observations the jet appears to dominate the spectral energy distribution (SED) from radio to IR. We model the evolution of the jet SED during this outburst using the internal-shock model implemented in the ISHEM code (Malzac 2014). In this model, the jet emission results from shocks triggered by fast fluctuations of the ejection velocity. The shape of the SED is almost entirely determined by the power spectrum of these fluctuations. The other jet parameters can only shift the SED in photon frequency or in normalisation. These fluctuations of velocity may be related to the variability of the accretion flow, which is best traced using the X-ray light curves. For this reason, we use the observed X-ray power spectra as input to our model to calculate the jet SED for five different luminosities and spectral shapes. We show that the model successfully matches the observed SEDs. In order to reproduce the spectral evolution we need to vary at least 2 parameters. I propose a scenario in which both the jet power and (time-averaged) Lorentz factor increase with the luminosity of the source. Our results are compatible with the variations of the jet Lorentz factor tested in an earlier study of this source (Russell et al. 2015). However, due to the large degeneracy in the other parameters of the model, this scenario is not unique.

Pdf file

Back to previous page