A full spectral-timing model to map the accretion flow in black hole binaries: the low/hard state of MAXI J1820+070. (arXiv:2107.12517v3 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Kawamura_T/0/1/0/all/0/1">Tenyo Kawamura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Axelsson_M/0/1/0/all/0/1">Magnus Axelsson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Done_C/0/1/0/all/0/1">Chris Done</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takahashi_T/0/1/0/all/0/1">Tadayuki Takahashi</a>
The nature and geometry of the accretion flow in the low/hard state of black
hole binaries is currently controversial. While most properties are generally
explained in the truncated disc/hot inner flow model, the detection of a broad
residual around the iron line argues for strong relativistic effects from an
untruncated disc. Since spectral fitting alone is somewhat degenerate, we
combine it with the additional information in the fast X-ray variability and
perform a full spectral-timing analysis for NICER and NuSTAR data on a bright
low/hard state of MAXI J1820+070. We model the variability with propagating
mass accretion rate fluctuations by combining two separate current insights:
that the hot flow is spectrally inhomogeneous, and that there is a
discontinuous jump in viscous time-scale between the hot flow and variable
disc. Our model naturally gives the double-humped shape of the power spectra,
and the increasing high-frequency variability with energy in the second hump.
Including reflection and reprocessing from a disc truncated at a few tens of
gravitational radii quantitatively reproduces the switch in the lag-frequency
spectra, from hard lagging soft at low frequencies (propagation through the
variable flow) to the soft lagging hard at the high frequencies (reverberation
from the hard X-ray continuum illuminating the disc). The viscous time-scale of
the hot flow is derived from the model, and we show how this can be used to
observationally test ideas about the origin of the jet.
The nature and geometry of the accretion flow in the low/hard state of black
hole binaries is currently controversial. While most properties are generally
explained in the truncated disc/hot inner flow model, the detection of a broad
residual around the iron line argues for strong relativistic effects from an
untruncated disc. Since spectral fitting alone is somewhat degenerate, we
combine it with the additional information in the fast X-ray variability and
perform a full spectral-timing analysis for NICER and NuSTAR data on a bright
low/hard state of MAXI J1820+070. We model the variability with propagating
mass accretion rate fluctuations by combining two separate current insights:
that the hot flow is spectrally inhomogeneous, and that there is a
discontinuous jump in viscous time-scale between the hot flow and variable
disc. Our model naturally gives the double-humped shape of the power spectra,
and the increasing high-frequency variability with energy in the second hump.
Including reflection and reprocessing from a disc truncated at a few tens of
gravitational radii quantitatively reproduces the switch in the lag-frequency
spectra, from hard lagging soft at low frequencies (propagation through the
variable flow) to the soft lagging hard at the high frequencies (reverberation
from the hard X-ray continuum illuminating the disc). The viscous time-scale of
the hot flow is derived from the model, and we show how this can be used to
observationally test ideas about the origin of the jet.
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