Other
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.0903w&link_type=abstract
American Astronomical Society, HEAD meeting #9, #9.03; Bulletin of the American Astronomical Society, Vol. 38, p.363
Other
Scientific paper
Chandra observations of radio galaxies have identified many cases where the X-ray jet emission on kpc scales is dominated by synchrotron radiation. The short electron radiation lifetimes require in situ particle acceleration, a condition not required for radio emission alone. Polarization data indicate magnetic field structures, and help to separate the flows of higher- and lower-energy electrons if measurements are available both in the optical and radio.
We will present observations that illustrate both the knotty and more continuous nature of the X-ray synchrotron emission in jets. Some knots are broadly as expected, where strong shocks associated with transverse magnetic fields are likely to be responsible for particle acceleration. 3C 15 is such an example, where the widths of the main envelopes of optical and radio emission, combined with the polarization-vector directions, are consistent with the jet containing a faster spine and slower sheath. In other cases, the magnetic-field vectors have a greater tendency to lie roughly parallel to lines of jet knots. In one case, 3C 346, we describe how this is likely to be due to an oblique shock formed by the interaction of the jet with the external medium, a result which disfavors a ballistic model for the jet. In NGC 315, a helical strand of enhanced radio and X-ray synchrotron emission can be interpreted as lying in the shear layer between faster inner and slower outer flows, in which case it may be bright either due to a superposition of Kelvin-Helmholtz-instability surface modes, or due to magnetic field and particles injected into the flow.
Birkinshaw Mark
Bridle Alan H.
Cotton William D.
Dulwich Fred
Laing Robert A.
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