Baryon Loading Efficiency and Particle Acceleration Efficiency of Relativistic Jets: Cases for Low Luminosity Bl Lacs

Abstract

Relativistic jets launched by supermassive black holes, so-called as active galactic nuclei (AGNs), are known as the most energetic particle accelerators in the universe. However, the baryon loading efficiency onto the jets from the accretion flows and their particle acceleration efficiencies have been veiled in mystery. With the latest data sets, we perform multi-wavelength spectral analysis of quiescent spectra of 13 TeV gamma-ray detected high-frequency-peaked BL Lacs (HBLs) following one-zone static synchrotron-self-Compton (SSC) model. We determine the minimum, cooling break, and maximum electron Lorentz factors following the diffusive shock acceleration (DSA) theory. We find that HBLs have P B /P e ∼ 6.3 × 10 −3 and the radiative efficiency ǫ rad,jet ∼ 6.7 × 10 −4 where P B and P e is the Poynting and electron power, respectively. By assuming 10 leptons per one proton, the jet power relates to the black hole mass as P jet /L Edd ∼ 0.18 where P jet and L Edd is the jet power and the Eddington luminosity, respectively. Under our model assumptions, we further find that HBLs have the jet production efficiency of η jet ∼ 1.5 and the mass loading efficiency of ξ jet 5 × 10 −2 . We also investigate the particle acceleration efficiency in the blazar zone by including the most recent Swift/BAT data. Our samples ubiquitously have the particle acceleration efficiency of η g ∼ 10 4.5 , which is inefficient to accelerate particles up to the ultra-high-energy-cosmic-ray (UHECR) regime. This implies that the UHECR acceleration sites should be other than the blazar zones of quiescent low power AGN jets, if one assumes the one-zone SSC model based on the DSA theory.

Disk–Jet Connection in Active Supermassive Black Holes in the Standard Accretion Disk Regime

“…Celotti & Ghisellini 2008;Ghisellini et al 2014;Inoue & Tanaka 2016), while our results show η jet 1.1…”

“…Celotti & Ghisellini 2008;Ghisellini et al 2014;Inoue & Tanaka 2016). Different from our radio quasar studies, blazar studies enable us to compare accretion with jet outflow at the same epoch.…”

“…Inoue & Tanaka 2016;Pjanka et al 2016). More pairs per one proton and/or higher γ e,min would reduce the jet power estimation based on blazar spectral fit.…”

Magnetic energy dissipation and origin of non-thermal spectra in radiatively efficient relativistic sources

“…Even though both these conditions are naturally expected in a fast cooling turbulent plasma (see Section 3.2), providing a fully convincing interpretation remains difficult. Indeed, two main inconsistencies arise: under the assumption that the electron distribution is isotropic, fitting the SED indicates that (i) U B U e , so that the jet should be matter dominated even if the proton component is completely absent; (ii) γ cool γ b , so that the role of cooling in shaping the electron energy distribution should be negligible (Tavecchio & Ghisellini 2016; see also Inoue & Tanaka 2016;Nalewajko & Gupta 2017;Costamante et al 2018). 2 2 Note that, if the non-thermal electrons in BL Lacs are not cooling efficiently (γ cool γ b ) and the break is therefore not due to cooling, one would need an acceleration mechanism that produces (i) an electron energy distribution dn e /dγ ∝ γ −2 at low energies; (ii) an energy distribution dn e /dγ ∝ γ −p with p > 2 at high energies.…”

Linear theory of the Rayleigh–Taylor instability at a discontinuous surface of a relativistic flow

“…Multiple outflow layers inside a relativistic jet are essential for reproducing the typical observed spectra of GRBs (Ito et al 2014). The development of turbulence inside the jet is an important issue in any discussion of the mechanism for efficient particle acceleration in the context of GRBs (Asano & Terasawa 2015) and blazars (Asano & Hayashida 2015;Inoue & Tanaka 2016).…”