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Revisiting the structure and spectrum of the magnetic-reconnection-heated corona in luminous AGNs | | J. Y. Liu
; ErLin Qiao
; B. F. Liu
; | | Date: |
22 Nov 2016 | | Abstract: | It is believed that the hard X-ray emission in the luminous active galactic
nuclei (AGNs) is from the hot corona above the cool accretion disk. However,
the formation of the corona is still debated. Liu et al. investigated the
spectrum of the corona heated by the reconnection of the magnetic field
generated by dynamo action in the thin disk and emerging into the corona as a
result of buoyancy instability. In the present paper, we improve this model to
interpret the observed relation of the hard X-ray spectrum becoming softer at
higher accretion rate in luminous AGNs. The magnetic field is characterized by
$eta_{
m 0}$, i.e., the ratio of the sum of gas pressure and radiation
pressure to magnetic pressure in the disk ($eta_{
m 0}=(P_{
m g,d}+P_{
m
r,d})/P_{
m B}$). Besides, both the intrinsic disk photons and reprocessed
photons by the disk are included as the seed photons for inverse Compton
scattering. These improvements are crucial for investigating the effect of
magnetic field on the accretion disk-corona when it is not clear whether the
radiation pressure or gas pressure dominates in thin disk. We change the value
of $eta_{
m 0}$ in order to constrain the magnetic field in the accretion
disk. We find that the energy fraction released in the corona ($f$) gradually
increases with the decrease of $eta_{
m 0}$ for the same accretion rate.
When $eta_{
m 0}$ decreases to less than 50, the structure and spectrum of
the disk-corona is independent on accretion rate, which is similar to the hard
spectrum found in Liu et al.(2003). Comparing with the observational results of
the hard X-ray bolometric correction factor in a sample of luminous AGNs, we
suggest that the value of $eta_{
m 0}$ is about 100-200 for $alpha=0.3$ and
the energy fraction $f$ should be larger than $30\%$ for hard X-ray emission. | | Source: | arXiv, 1611.7149 | | Services: | Forum | Review | PDF | Favorites | |
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