MOMENTUM DRIVING: WHICH PHYSICAL PROCESSES DOMINATE ACTIVE GALACTIC NUCLEUS FEEDBACK?

By Jeremiah P. Ostriker, E. Choi, Luca Ciotti, G. Novak, D. Proga. 2010

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The deposition of mechanical feedback from a supermassive black hole (SMBH) in an active galactic nucleus into the surrounding galaxy occurs via broad-line winds which must carry mass and radial momentum as well as energy. The effect can be summarized by the dimensionless parameter where ϵw is the efficiency with which accreted matter is turned into wind energy in the disk surrounding the central SMBH. The outflowing mass and momentum are proportional to η, and many prior treatments have essentially assumed that η = 0. We perform one- and two-dimensional simulations and find that the growth of the central SMBH is very sensitive to the inclusion of the mass and momentum driving but is insensitive to the assumed mechanical efficiency. For example in representative calculations, the omission of momentum and mass feedback leads to a hundred-fold increase in the mass of the SMBH to over 1010 M☉. When allowance is made for momentum driving, the final SMBH mass is much lower and the wind efficiencies that lead to the most observationally acceptable results are relatively low with ϵw ≲ 10−4.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/04e8deb375cb48b8d1fe1f408250811c14c1b85d

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Citations in the corpus

Hot Accretion Flows Around Black Holes (2014, background): “However, momentum feedback can more effectively push the surrounding gas and may be equally important for controlling the growth of the black hole and switching off star formation (King 2003, 2005, 2010; Ostriker et al. 2010; Debuhr et al. 2010; Silk 2013).”
NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. II. NATURE, ORIGIN, AND PROPERTIES OF OUTFLOWS AND THEIR POSSIBLE OBSERVATIONAL APPLICATIONS (2012, background): “For example, Ostriker et al. (2010) have shown that the growth of the central supermassive black hole in galactic center is mainly determined by the mass and momentum feedback of outflow.”
Unification of X-ray winds in Seyfert galaxies: from ultra-fast outflows to warm absorbers (2012, background): “…to significantly influence the bulge evolution, star formation, super-massive black hole growth and contribute to the establishment of the observed black hole-host galaxy relations, such as the MBH–σ (Ferrarese & Merritt 2000; King 2010a; Ostriker et al. 2010; Gaspari et al. 2011a, b, 2012a, b).”
Theoretical Challenges in Galaxy Formation (2016, background): “First, there is no physical means specified for communicating the energy from the black holes to the surrounding gas in these treatments (see discussion in Ostriker et al. 2010).”
Energy, momentum and mass outflows and feedback from thick accretion discs around rotating black holes (2013, background): “The former is traditionally considered in cosmological simulations (e.g. Di Matteo et al. 2005; Springel et al. 2005), but the latter may also be important (King 2003, 2010; Debuhr et al. 2010; Ostriker et al. 2010).”
Galacticus: A Semi-Analytic Model of Galaxy Formation (2010, background): “…if the cooling radius is smaller than the virial radius; see, for example, Benson and Bower 2010a); Quasar-mode A mechanical wind luminosity of (Ostriker et al., 2010) Lwind = •,wind Ṁ0c2, (3) where •,wind =[blackHoleWindEfficiency] is the black hole wind efficiency, is added to the gas…”
Quasar outflows and AGN feedback in the extreme UV: HST/COS observations of HE 0238−1904 (2013, background): “The energy, mass, and momentum carried by these outflows are thought to play an important role in shaping the early universe and dictating its evolution (e.g. Scannapieco & Oh 2004; Levine & Gnedin 2005; Hopkins et al. 2006; Cattaneo et al. 2009; Ciotti et al. 2009, 2010; Ostriker et al. 2010).”
FEEDBACK FROM CENTRAL BLACK HOLES IN ELLIPTICAL GALAXIES. III. MODELS WITH BOTH RADIATIVE AND MECHANICAL FEEDBACK (2010, methodology): “This means that a proper description of SMBH feedback requires both the physical components, as discussed in detail in Ostriker et al. 2010.”
NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. III. REVISITING WIND PROPERTIES USING THE TRAJECTORY APPROACH (2015, background): “…flow is one of the most important ingredients for such a feedback because they could interact with the ISM in the host galaxy by exchanging momentum and depositing energy (King 2003; Debuhr et al. 2010; Ciotti, Ostriker & Proga 2010; Ostriker et al. 2010; Novak et al. 2011; Gan et al. 2014).”
Physical Models of Galaxy Formation in a Cosmological Framework (2014, background): “It has been argued that in the dense cold gas that must surround rapidly accreting black holes, cooling times are short and winds must be predominantly momentum-driven (Debuhr et al. 2011, King 2005, Ostriker et al. 2010).”
FEEDBACK FROM CENTRAL BLACK HOLES IN ELLIPTICAL GALAXIES: TWO-DIMENSIONAL MODELS COMPARED TO ONE-DIMENSIONAL MODELS (2010, background): “As discussed in detail in Ostriker et al. (2010), these expressions guarantee that the mass, energy, and momentum carried by the wind are selfconsistent.”
Relativistic jet feedback – III. Feedback on gas discs (2018, background): “Such winds are primarily considered to be wide-angled, driven by the radiation pressure from the luminous AGN (e.g. Proga 2000; Ostriker et al. 2010; Bieri et al. 2017).”
Mechanical AGN feedback: controlling the thermodynamical evolution of elliptical galaxies (2012, background): “Many fundamental questions about the physics of AGN feedback, however, remain unanswered (see also Ostriker et al. 2010).”
DRIVING OUTFLOWS WITH RELATIVISTIC JETS AND THE DEPENDENCE OF ACTIVE GALACTIC NUCLEUS FEEDBACK EFFICIENCY ON INTERSTELLAR MEDIUM INHOMOGENEITY (2012, background): “The feedback requires relatively high injection rates of thermal energy, compared to a wind that is dominated by kinetic energy and can drive the bubble through ram pressure as well thermal pressure (Ostriker et al. 2010).”
THE COSMOLOGICAL SIZE AND VELOCITY DISPERSION EVOLUTION OF MASSIVE EARLY-TYPE GALAXIES (2011, background): “…AGN feedback (e.g Sazonov et al. 2004; Di Matteo et al. 2005; Springel et al. 2005; Johansson et al. 2009a; Booth & Schaye 2009; Debuhr et al. 2010; Ostriker et al. 2010; Schaye et al. 2010), radiative feedback from stars (e.g Oppenheimer & Davé 2006; Petkova & Springel 2009; Hopkins et al. 2011)…”