2012/09/20 by L. E. H. Godfrey, L. Godfrey, J. E. J. Lovell +15 · 1 voice · 1 citation
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics and Cosmic Phenomena #Gamma-ray bursts and supernovae #astro-ph.CO #astro-ph.HE
paper · pdf · doi:10.1088/2041-8205/758/2/l27
openalex publication_date 2012/09/27 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/01
We present 18 GHz Australia Telescope Compact Array imaging of the megaparsec-scale quasar jet PKS 0637−752 with angular resolution ∼0 58. We draw attention to a spectacular train of quasi-periodic knots along the inner 11'' of the jet, with average separation ∼1.1 arcsec (7.6 kpc projected). We consider two classes of model to explain the periodic knots: those that involve a static pattern through which the jet plasma travels (e.g., stationary shocks) and those that involve modulation of the jet engine. Interpreting the knots as re-confinement shocks implies the jet kinetic power Q jet ∼ 10 46 erg s −1 , but the constant knot separation along the jet is not expected in a realistic external density profile. For models involving modulation of the jet engine, we find that the required modulation period is 2 × 10 3 yr < τ < 3 × 10 5 yr. The lower end of this range is applicable if the jet remains highly relativistic on kiloparsec scales, as implied by the IC/CMB model of jet X-ray emission. We suggest that the periodic jet structure in PKS 0637−752 may be analogous to the quasi-periodic jet modulation seen in the microquasar GRS 1915+105, believed to result from limit cycle behavior in an unstable accretion disk. If variations in the accretion rate are driven by a binary black hole, the predicted orbital radius is 0.7 pc ≲ a ≲ 30 pc, which corresponds to a maximum angular separation of ∼0.1–5 mas.