A global view of the inner accretion/ejection flow around super massive black holes: radiation driven accretion disk winds in a physical context. (arXiv:1904.07341v1 [astro-ph.GA])

A global view of the inner accretion/ejection flow around super massive black holes: radiation driven accretion disk winds in a physical context. (arXiv:1904.07341v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Giustini_M/0/1/0/all/0/1">Margherita Giustini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Proga_D/0/1/0/all/0/1">Daniel Proga</a>

Understanding the physics and geometry of accretion and ejection around super
massive black holes (SMBHs) is important to understand the evolution of active
galactic nuclei (AGN) and therefore of the large scale structures of the
Universe. We aim at providing a simple, coherent, and global view of the
sub-parsec accretion/ejection flow in AGN with varying Eddington ratio,
$dot{m}$ and black hole mass, $M_{BH}$. We make use of theoretical insights,
results of numerical simulations, as well as UV/X-ray observations to review
the inner regions of AGN by including different accretion/ejection modes, with
special emphasis on the role of radiation in driving powerful accretion disk
winds from the inner regions around the central SMBH. We propose five $dot{m}$
regimes where the physics of the inner accretion/ejection flow around SMBHs is
expected to change, and that correspond observationally to quiescent/inactive
galaxies, LLAGN, Seyferts/mini-BAL QSOs, NLS1s/BAL QSOs, and super-Eddington
sources. We include in this scenario radiation driven disk winds, that are
strong in the high $dot{m}$, large $M_{BH}$ regime, and possibly present but
likely weak in the moderate $dot{m}$, small $M_{BH}$ regime. A great diversity
of the accretion/ejection flows in AGN can be explained to a good degree by
varying just two fundamental properties: the Eddington ratio $dot{m}$ and the
black hole mass $M_{BH}$, and by the inclusion of accretion disk winds that can
naturally be launched by the radiation emitted from luminous accretion disks.

Understanding the physics and geometry of accretion and ejection around super
massive black holes (SMBHs) is important to understand the evolution of active
galactic nuclei (AGN) and therefore of the large scale structures of the
Universe. We aim at providing a simple, coherent, and global view of the
sub-parsec accretion/ejection flow in AGN with varying Eddington ratio,
$dot{m}$ and black hole mass, $M_{BH}$. We make use of theoretical insights,
results of numerical simulations, as well as UV/X-ray observations to review
the inner regions of AGN by including different accretion/ejection modes, with
special emphasis on the role of radiation in driving powerful accretion disk
winds from the inner regions around the central SMBH. We propose five $dot{m}$
regimes where the physics of the inner accretion/ejection flow around SMBHs is
expected to change, and that correspond observationally to quiescent/inactive
galaxies, LLAGN, Seyferts/mini-BAL QSOs, NLS1s/BAL QSOs, and super-Eddington
sources. We include in this scenario radiation driven disk winds, that are
strong in the high $dot{m}$, large $M_{BH}$ regime, and possibly present but
likely weak in the moderate $dot{m}$, small $M_{BH}$ regime. A great diversity
of the accretion/ejection flows in AGN can be explained to a good degree by
varying just two fundamental properties: the Eddington ratio $dot{m}$ and the
black hole mass $M_{BH}$, and by the inclusion of accretion disk winds that can
naturally be launched by the radiation emitted from luminous accretion disks.

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