Jet Trails and Mach Cones: The Interaction of Microquasars with the Interstellar Medium
Yoon, D. ( Department of Astronomy, University of Wisconsin-Madison, Madison, WI, USA ); Morsony, B. ( Department of Astronomy, University of Wisconsin-Madison, Madison, WI, USA ); Heinz, S. ( Department of Astronomy, University of Wisconsin-Madison, Madison, WI, USA ); Wiersema, K. ( Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH, UK ); Fender, R. P. ( School of Physics & Astronomy, University of Southampton, Highfield, Southampton, S017 1BJ, UK ); Russell, D. M. ( Astronomical Institute Anton Pannekoek, University of Amsterdam, P.O. Box 94249, 1090 GE Amsterdam, The Netherlands ); Sunyaev, R. ( Space Research Institute (IKI), Moscow, Russia ; Max-Plank-Institut für Astrophysik, Garching, Germany ) show affiliations
The Astrophysical Journal, Volume 742, Issue 1, article id. 25, 16 pp. (2011).
Published in Nov 2011
A subset of microquasars exhibits high peculiar velocity with respect to the local standard of rest due to the kicks they receive when being born in supernovae. The interaction between the radio plasma released by microquasar jets from such high-velocity binaries with the interstellar medium must lead to the production of trails and bow shocks similar to what is observed in narrow-angle tailed radio galaxies and pulsar wind nebulae. We present a set of numerical simulations of this interaction that illuminate the long-term dynamical evolution and the observational properties of these microquasar bow-shock nebulae and trails. We find that this interaction always produces a structure that consists of a bow shock, a trailing neck, and an expanding bubble. Using our simulations to model emission, we predict that the shock surrounding the bubble and the neck should be visible in Hα emission, the interior of the bubble should be visible in synchrotron radio emission, and only the bow shock is likely to be detectable in X-ray emission. We construct an analytic model for the evolution of the neck and bubble shape and compare this model with observations of the X-ray binary SAX J1712.6-3739.
Astronomy: ISM: jets and outflows; X-rays: binaries
arXiv: Astrophysics - High Energy Astrophysical Phenomena