Radio structure of the blazar 1156+295 with sub-pc resolution

TL;DR

This study uses multi-frequency VLBA observations to analyze the innermost jet structure of the blazar 1156+295, revealing a helical jet pattern likely driven by Kelvin-Helmholtz instability, with implications for understanding jet dynamics.

Contribution

First detailed multi-epoch, multi-frequency VLBA imaging of 1156+295's inner jet, supporting a hydrodynamic helical jet model based on Kelvin-Helmholtz instability.

Findings

Jet components exhibit superluminal motion between 3.6c and 11.6c.

Jet morphology shows oscillatory, helical patterns.

Kelvin-Helmholtz instability model fits observed jet structure.

Abstract

1156+295 is a flat-spectrum quasar which is loud at radio and gamma-ray. Previous observations of the source revealed a radio morphology on pc to kpc scales consistent with a helical jet model. In our present research, this source was observed with the VLBA at 86, 43 and 15 GHz on four epochs from 10 May 2003 to 13 March 2005 aiming at studying the structure of the innermost jet in order to understand the relation between the helical structure and the astrophysical processes in the central engine. A core-jet structure with six jet components is identified. The apparent transverse velocities of the six jet components derived from proper motion measurements are in the range between 3.6 c and 11.6 c. The overall jet shape shows oscillatory morphology with multiple curvatures on pc scales which might be indicative of a helical pattern. Models of helical jet are discussed on the basis of both Kelvin-Helmholtz (K-H) instability and jet precession. The K-H instability model shows better agreement with the observed data. The overall radio structure on the scale from sub-pc to kpc appears to be fitted with a hydrodynamic model with the fundamental helical mode in Kelvin-Helmholtz (K-H) instability. This helical mode with an initial characteristic wavelength of 0.2 pc is excited at the base of the jet on the scale of 0.005 pc (or 1000R_s, the typical size of the broad line region for a super massive black hole of $4.3\times10^8M_{\odot}$). A presessing jet model can also fit the observed jet structure on the scale between 10 pc and 300 pc. However, additional astrophysical processes may be required for the presessing jet model in order to explain the bendings on the inner jet structure (1 to 10 pc) and re-collimation of the large scale jet outflow (>300 pc).