Winds from Black Hole Accretion Flows: Formation and Their Interaction with ISM

Yuan, Feng

doi:10.1007/978-3-662-52859-4_4

Cited by 1 publication

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“…Here we only briefly summarize the main development and readers are referred to the recent review by Yuan (2016) for more details. In the pioneer work of Narayan & Yi (1994), it has been speculated that strong outflow should be easily formed because of the positive Bernoulli parameter of the hot accretion flow.…”

Section: Introductionmentioning

confidence: 99%

Radiative Heating in the Kinetic Mode of AGN Feedback

Xie

Yuan

2017

ApJ

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AGN feedback is now widely believed to play a crucial role in the co-evolution between the central black hole and its host galaxy. Two feedback modes have been identified, namely the radiative and kinetic modes, which correspond to the luminous AGNs and low-luminosity AGNs (LLAGNs), respectively. In this paper, we investigate the radiative heating in the kinetic mode. This process is potentially important because: 1) the radiation power of LLAGNs is higher than the jet power over a wide parameter range; 2) the spectral energy distribution of LLAGNs is such that the radiative heating is more effective compared to that of luminous AGNs with the same luminosity; and 3) most of the time in the lifecycle of an AGN is spent in the LLAGNs phase. In this paper, adopting the characteristic broad-band spectral energy distributions of LLAGNs, we calculate the value of "Compton temperature" (T C ), which determines the radiative heating by Compton scattering. We find that T C ∼ (5 − 15) × 10 7 K, depending on the spectrum of individual LLAGN and at which distance from the black hole we evaluate the heating. We also compare this heating process with other radiative heating and cooling processes such as photoionization/recombination. Our result can be used for an accurate calculation of the radiative heating in the study of AGN feedback.

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Section: Introductionmentioning

confidence: 99%