Powers and Magnetization of Blazar Jets

Sikora, Marek

doi:10.3390/galaxies4030012

Cited by 21 publications

(15 citation statements)

References 48 publications

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“…The results manifest that the jet of blazar contains an important fraction of eletron/positron pairs, with n pairs /n p ∼ 10 (left panel in Figure 2). Our results are consistent with previous works, where they pointed out that the electron/positron pairs were important on the number density in blazar jet (Kang et al 2014;Sikora 2016;Pjanka et al 2017). The ratio 10 pairs per proton is also consistent with the upper limit for pairs to avoid the Compton rocket effect Ghisellini 2012).…”

Section: Discussionsupporting

confidence: 93%

Constraints on the Composition, Magnetization, and Radiative Efficiency in the Jets of Blazars

Fan

Liao³

2018

ApJ

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The composition and energy dissipation in jets are two of the fundamental questions of jet physics that are not fully understood. In this paper, we attempt to constrain the composition, magnetization as well as radiative efficiency for blazar with the recently released low-frequency radio catalog of the TIFR GMRT Sky Survey at 150 MHz. The jet power estimated from the low-frequency radio emission is much lower than that derived from spectral energy distribution fitting assuming one proton per electron. Assuming the jet power estimated from low-frequency radio emission is physical, the fraction of electron/positron pairs can be constrained with n pairs /n p ∼ 10. By comparing the power carried by magnetic field and radiation with the jet power estimated from the low-frequency radio emission, we find both relatively high magnetization parameter of σ ∼ 0.5 and radiative efficiency of η ∼ 0.4 in the dissipation region of blazars. These results suggest that the magnetic reconnection processes may play an important role in the energy dissipation of blazars. We also explore the connection between these three parameters (n pairs /n p , σ, and η) and the black hole mass, disk luminosity as well as Eddington ratio. No significant correlation is found, except that σ shows possible correlation with disk luminosity.

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Section: Discussionsupporting

confidence: 93%

Constraints on the Composition, Magnetization, and Radiative Efficiency in the Jets of Blazars

Fan

Liao³

2018

ApJ

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“…However, even for the strictly leptonic SED models, and even in the limit of completely cold protons, the contribution of protons to the total jet power can be dominant, provided that γe < (np/ne)(mp/me), where ne = (n e + ) + (n e − ). In the case of no pairs (np = ne), the powers of blazar jets calculated by Ghisellini et al (2014) are found to exceed by a factor ∼ 20 the jet powers estimated using the calorimetry of radio lobes (Kang et al 2014;Sikora 2016;Pjanka et al 2017;Fan et al 2018) and radio core shifts studies (Pjanka et al 2017).…”

Section: Introductionmentioning

confidence: 82%

On the significance of relativistically hot pairs in the jets of FR II radio galaxies

Sikora,

Nalewajko,

Madejski

2020

Preprint

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The energetic composition of radio lobes in the FR II galaxies -estimated by comparing their radio luminosities with the powers required to inflate cavities in the external medium -seems to exclude the possibility of their energetic domination by protons. Furthermore, if the jets were dominated by the kinetic energy of cold protons, it would be difficult to efficiently accelerate leptons in the jets' terminal shocks. This suggests that the jets powering the lobes are dominated by pairs not only in number but also in enthalpy. Such a possibility is confronted against the constraints imposed by the jet formation scenarios, and by the properties of jets on parsec and kiloparsec scales. We find a lower limit on the pair content from the energetic dominance of leptons over protons in the radio lobes, which exceeds the estimate of n e /n p ∼ 20 indicated by models of the blazar zones and of the radio cores. This allows us to establish that the average energy of protons in the jet co-moving frame is < 2m p c 2 , and to estimate the number fluxes of protons and e + e − pairs. The required proton flux is achievable, if the jet carries away about 1% of the accreting matter. Loading the jets by pairs can be achieved by pair creation using soft γ-ray photons from the accretion disk corona, provided that about 2-3% of the disk radiation extends beyond 1 MeV. Finally, we discuss possible dissipative mechanisms which may keep the jets dominated by relativistically hot pairs.

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“…Therefore, our result supports the BZ mechanism for jet launching The magnetization and radiative efficiency are usually considered to be the indicator of acceleration mechanism occurring in blazar jets. We derive the magnetization parameter σB and radiative efficiency ηr (Kang et al 2014;Sikora 2016;Fan et al 2018),…”

Section: On the Magnetization And Radiative Efficiencymentioning

confidence: 99%

On the injection of relativistic electrons in the jet of 3C 279

Yan

Dai

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The acceleration of electrons in 3C 279 is investigated through analyzing the injected electron energy distribution (EED) in a time-dependent synchrotron self-Compton + external Compton emission model. In this model, it is assumed that relativistic electrons are continuously injected into the emission region, and the injected EED [Q ′ e (γ ′ )] follows a single power-law form with low-and high-energy cutoffs γ ′ min and γ ′ max , respectively, and the spectral index n, i.e, Q ′ e (γ ′ ) ∝ γ ′−n . This model is applied to 14 quasi-simultaneous spectral energy distributions (SEDs) of 3C 279. The Markov Chain Monte Carlo fitting technique is performed to obtain the best-fitting parameters and the uncertainties on the parameters. The results show that the injected EED is well constrained in each state. The value of n is in the range of 2.5 to 3.8, which is larger than that expected by the classic non-relativistic shock acceleration. However, the large value of n can be explained by the relativistic oblique shock acceleration. The flaring activity seems to be related to an increased acceleration efficiency, reflected in an increased γ ′ min and electron injection power.

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Powers and Magnetization of Blazar Jets

Cited by 21 publications

References 48 publications

Constraints on the Composition, Magnetization, and Radiative Efficiency in the Jets of Blazars

Constraints on the Composition, Magnetization, and Radiative Efficiency in the Jets of Blazars

On the significance of relativistically hot pairs in the jets of FR II radio galaxies

On the injection of relativistic electrons in the jet of 3C 279

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