Cookies

We use cookies to ensure that we give you the best experience on our website. You can change your cookie settings at any time. Otherwise, we'll assume you're OK to continue.

Department of Physics

Staff profile

Publication details for Dr Alastair Edge

Snios, Bradford, Nulsen, Paul E. J., Wise, Michael W., de Vries, Martijn, Birkinshaw, Mark, Worrall, Diana M., Duffy, Ryan T., Kraft, Ralph P., McNamara, Brian R., Carilli, Chris, Croston, Judith H., Edge, Alastair C., Godfrey, Leith E. H., Hardcastle, Martin J., Harris, Daniel E., Laing, Robert A., Mathews, William G., McKean, John P., Perley, Richard A., Rafferty, David A. & Young, Andrew J. (2018). The Cocoon Shocks of Cygnus A: Pressures and Their Implications for the Jets and Lobes. The Astrophysical Journal 855(1): 71.

Author(s) from Durham

Abstract

We use 2.0 Msec of Chandra observations to investigate the cocoon shocks of Cygnus A and some implications for its lobes and jet. Measured shock Mach numbers vary in the range 1.18–1.66 around the cocoon. We estimate a total outburst energy of $\simeq 4.7\times {10}^{60}\,\mathrm{erg}$, with an age of $\simeq 2\times {10}^{7}\,\mathrm{years}$. The average postshock pressure is found to be $8.6\pm 0.3\times {10}^{-10}\,\mathrm{erg}\,{\mathrm{cm}}^{-3}$, which agrees with the average pressure of the thin rim of compressed gas between the radio lobes and shocks, as determined from X-ray spectra. However, average rim pressures are found to be lower in the western lobe than in the eastern lobe by sime20%. Pressure estimates for hotspots A and D from synchrotron self-Compton models imply that each jet exerts a ram pressure gsim3 times its static pressure, consistent with the positions of the hotspots moving about on the cocoon shock over time. A steady, one-dimensional flow model is used to estimate jet properties, finding mildly relativistic flow speeds within the allowed parameter range. Models in which the jet carries a negligible flux of rest mass are consistent with the observed properties of the jets and hotspots. This favors the jets being light, implying that the kinetic power and momentum flux are carried primarily by the internal energy of the jet plasma rather than by its rest mass.