Migliari, SimoneFender, R. P.Blundell, K. N.Méndez, M.Van der Klis, M.2016-06-132016-06-132005-010035-8711https://hdl.handle.net/2445/99488We present X-ray images of all the available Chandra observations of the galactic jet source SS 433. We have studied the morphology of the X-ray images and inspected the evolution of the arcsec X-ray jets, recently found to be manifestations of in situ reheating of the relativistic gas downstream in the jets. The Chandra images reveal that the arcsec X-ray jets are not steady long-term structures; the structure varies, indicating that the reheating processes have no preference for a particular precession phase or distance from the binary core. Three observations made within about five days in 2001 May, and a 60-ks observation made in 2003 July, show that the variability of the jets can be very rapid, from time-scales of days to (possibly) hours. The three 2001 May images show two resolved knots in the east jet getting brighter one after the other, suggesting that a common phenomenon might be at the origin of the sequential reheatings of the knots. We discuss possible scenarios and propose a model to interpret these brightenings in terms of a propagating shock wave, revealing a second, faster outflow in the jet.9 p.application/pdfeng(c) Migliari, Simone et al., 2005Astronomia de raigs XJets (Astrofísica)Estels binaris de raigs XRadioastronomiaX-ray astronomyAstrophysical jetsX-ray binariesRadio astronomyinfo:eu-repo/semantics/article6340362016-06-13info:eu-repo/semantics/openAccess