2013/03/26 by R. A. Laing, A. H. Bridle · 41 citations
Physics and Astronomy · #Acceleration #Active galactic nucleus #Amplitude #Astronomy #Astrophysical jet #Astrophysics #Astrophysics and Cosmic Phenomena #Classical mechanics #Flux (metallurgy) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Jet (fluid) #Luminosity #Mechanics #Optics #Particle acceleration #Physics #Radio Astronomy Observations and Technology #Radio galaxy #Spectral index #Spectral line #astro-ph.CO #astro-ph.HE
paper · pdf · doi:10.1093/mnras/stt531
published in Monthly Notices of the Royal Astronomical Society 432(2), 1114-1132 (Oxford University Press) · 21 pages, 9 figures, MNRAS, in press
arxiv created 2013/03/26 · openalex publication_date 2013/04/22 · arxiv updated 2015/06/15 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present accurate, spatially resolved imaging of radio spectra at the bases of jets in eleven low-luminosity (Fanaroff–Riley I) radio galaxies, derived from Very Large Array (VLA) observations. We pay careful attention to calibration and to the effects of random and systematic errors, and we base the flux-density scale on recent measurements of VLA primary amplitude calibrators by Perley and Butler. We show images and profiles of spectral index over the frequency range 1.4–8.5 GHz, together with values integrated over fiducial regions defined by our relativistic models of the jets. We find that the spectral index α, defined in the sense I(ν) ∝ ν−α, decreases with distance from the nucleus in all of the jets. The mean spectral indices are 0.66 ± 0.01 where the jets first brighten abruptly and 0.59 ± 0.01 after they recollimate. The mean change in spectral index between these locations, which is independent of calibration and flux-density scale errors and is therefore more accurately and robustly measured, is −0.067 ± 0.006. Our jet models associate the decrease in spectral index with a bulk deceleration of the flow from ≈0.8c to ≲ 0.5c. We suggest that the decrease is the result of a change in the characteristics of ongoing particle acceleration. One possible acceleration mechanism is the first-order Fermi process in mildly relativistic shocks: in the Bohm limit, the index of the electron energy spectrum, p = 2α + 1, is slightly larger than 2 and decreases with velocity upstream of the shock. This possibility is consistent with our measurements, but requires shocks throughout the jet volume rather than at a few discrete locations. A second possibility is that two acceleration mechanisms operate in these jets: one (with p = 2.32) dominant close to the galactic nucleus and associated with high flow speeds, another (with p = 2.18) taking over at larger distances and slower flow speeds.