Spectral signature of mass outflow in Two Component Advective Flow Paradigm. (arXiv:2107.13808v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Mondal_S/0/1/0/all/0/1">Santanu Mondal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chakrabarti_S/0/1/0/all/0/1">Sandip K. Chakrabarti</a>
Outflows are common in many astrophysical systems. In the Two Component
Advective Flow ({fontfamily{qcr}selectfont TCAF}) paradigm which is
essentially a generalized Bondi flow including rotation, viscosity and cooling
effects, the outflow is originated from the hot, puffed up, post-shock region
at the inner edge of the accretion disk. We consider this region to be the base
of the jet carrying away matter with high velocity. In this paper, we study the
spectral properties of black holes using {fontfamily{qcr}selectfont TCAF}
which includes also a jet ({fontfamily{qcr}selectfont JeTCAF}) in the
vertical direction of the disk plane. Soft photons from the Keplerian disk are
up-scattered by the post-shock region as well as by the base of the jet and are
emitted as hard radiation. We also include the bulk motion Comptonization
effect by the diverging flow of jet. Our self-consistent accretion-ejection
solution shows how the spectrum from the base of the jet varies with accretion
rates, geometry of the flow and the collimation factor of the jet. We apply the
solution to a jetted candidate GS,1354-64 to estimate its mass outflow rate
and the geometric configuration of the flow during 2015 outburst using {it
NuSTAR} observation. The estimated mass outflow to mass inflow rate is
$0.12^{+0.02}_{-0.03}$. From the model fitted accretion rates, shock
compression ratio and the energy spectral index, we identify the presence of
hard and intermediate spectral states of the outburst. Our model fitted jet
collimation factor ($f_{rm col}$) is found to be $0.47^{+0.09}_{-0.09}$.
Outflows are common in many astrophysical systems. In the Two Component
Advective Flow ({fontfamily{qcr}selectfont TCAF}) paradigm which is
essentially a generalized Bondi flow including rotation, viscosity and cooling
effects, the outflow is originated from the hot, puffed up, post-shock region
at the inner edge of the accretion disk. We consider this region to be the base
of the jet carrying away matter with high velocity. In this paper, we study the
spectral properties of black holes using {fontfamily{qcr}selectfont TCAF}
which includes also a jet ({fontfamily{qcr}selectfont JeTCAF}) in the
vertical direction of the disk plane. Soft photons from the Keplerian disk are
up-scattered by the post-shock region as well as by the base of the jet and are
emitted as hard radiation. We also include the bulk motion Comptonization
effect by the diverging flow of jet. Our self-consistent accretion-ejection
solution shows how the spectrum from the base of the jet varies with accretion
rates, geometry of the flow and the collimation factor of the jet. We apply the
solution to a jetted candidate GS,1354-64 to estimate its mass outflow rate
and the geometric configuration of the flow during 2015 outburst using {it
NuSTAR} observation. The estimated mass outflow to mass inflow rate is
$0.12^{+0.02}_{-0.03}$. From the model fitted accretion rates, shock
compression ratio and the energy spectral index, we identify the presence of
hard and intermediate spectral states of the outburst. Our model fitted jet
collimation factor ($f_{rm col}$) is found to be $0.47^{+0.09}_{-0.09}$.
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