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E. Kellogg, C. Anderson, J. DePasquale, K. Korreck, J. Nichols, J. Sokoloski (Harvard Smithsonian CfA), M. Krauss (Kavli Inst. MIT), J. Pedelty (NASA GSFC)
The symbiotic star R Aquarii has been known to emit collimated outflow in the form of jets for many years. We report on five years of observations in x-rays and radio using Chandra, VLA and XMM-Newton. We discuss the evolution of the outer thermal jets, including new observations performed in June and October 2005. We see motion of the NE x-ray jet at a projected velocity of about 600 km s-1. The SW x-ray jet has almost disappeared between 2000.7 and 2004.0. An XMM grating spectrum of the NE jet confirms the existence of O VII He-like lines, and offers the possibility of doing plasma density diagnostics. We comment on on the physics of cooling in the SW jet and implications for the density of the x-ray emitting gas, the heating mechanism, and mass and kinetic energy in the jets and its implications for the system as a whole. This work was supported by NASA and NSF.
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.