Radiation drag driven mass accretion in a clumpy interstellar medium: implications for the supermassive black hole-to-bulge relation

Kawakatu, Nozomu; Umemura, Masayuki

doi:10.1046/j.1365-8711.2002.05037.x

Cited by 55 publications

(74 citation statements)

References 40 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…One mechanism yielding such proportionality has been discussed by Umemura (2001), Kawakatu & Umemura (2002), and Kawakatu, Umemura, & Mori (2003). In the central regions of protogalaxies the drag due to stellar radiation may result in a loss of angular momentum of the gas at a rate that in a clumpy medium is well approximated by…”

Section: Black Hole Growthmentioning

confidence: 99%

A Physical Model for the Coevolution of QSOs and Their Spheroidal Hosts

Zotti¹,

Shankar²,

Lapi³

et al. 2004

ApJ

1,005

1,415

View full text Add to dashboard Cite

We present a physically motivated model for the early coevolution of massive spheroidal galaxies and active nuclei at their centers. Within dark matter halos, forming at the rate predicted by the canonical hierarchical clustering scenario, the gas evolution is controlled by gravity, radiative cooling, and heating by feedback from supernovae and from the growing active nucleus. Supernova heating is increasingly effective with decreasing binding energy in slowing down the star formation and in driving gas outflows. The more massive protogalaxies virializing at earlier times are thus the sites of the faster star formation. The correspondingly higher radiation drag fastens the angular momentum loss by the gas, resulting in a larger accretion rate onto the central black hole. In turn, the kinetic energy carried by outflows driven by active nuclei can unbind the residual gas, thus halting both the star formation and the black hole growth, in a time again shorter for larger halos. For the most massive galaxies the gas unbinding time is short enough for the bulk of the star formation to be completed before Type Ia supernovae can substantially increase the Fe abundance of the interstellar medium, thus accounting for the -enhancement seen in the largest galaxies. The feedback from supernovae and from the active nucleus also determines the relationship between the black hole mass and the mass, or the velocity dispersion, of the host galaxy, as well as the black hole mass function. In both cases the model predictions are in excellent agreement with the observational data. Coupling the model with GRASIL (Silva et al. 1998), the code computing in a selfconsistent way the chemical and spectrophotometric evolution of galaxies over a very wide wavelength interval, we have obtained predictions in excellent agreement with observations for a number of observables that proved to be extremely challenging for all the current semianalytic models, including the submillimeter counts and the corresponding redshift distributions, and the epoch-dependent K-band luminosity function of spheroidal galaxies.

show abstract

Section: Black Hole Growthmentioning

confidence: 99%

A Physical Model for the Coevolution of QSOs and Their Spheroidal Hosts

Zotti¹,

Shankar²,

Lapi³

et al. 2004

ApJ

1,005

1,415

View full text Add to dashboard Cite

show abstract

“…Several physical mechanisms can cause a fraction of the gas in galaxies to lose angular momentum and to pile up in the very central regions. A non exhaustive list includes gas drag, dynamical friction of gas plus star clumps, tidal fields, spiral waves, winds and bars, radiation drag (e.g., Norman & Scoville 1988;Shlosman et al 1989Shlosman et al , 1990Shlosman & Noguchi 1993;Hernquist & Mihos 1995;Noguchi 1999;Umemura 2001;Kawakatu & Umemura 2002;Kawakatu et al 2003;Thompson et al 2005;Bournaud et al 2007Bournaud et al , 2011, 2011. In general the presence of clumps, which may be generated by fragmentation of gas already organized in an unstable disc or by inflow of gas and star subclumps, tends to increase the efficiency of such mechanisms.…”

Section: The Reservoirmentioning

confidence: 99%

The Coevolution of Supermassive Black Holes and Massive Galaxies at High Redshift

Lapi

Raimundo

Aversa

et al. 2014

ApJ

114

View full text Add to dashboard Cite

We exploit the recent, wide samples of far-infrared (FIR) selected galaxies followed-up in X rays and of X-ray/optically selected active galactic nuclei (AGNs) followed-up in the FIR band, along with the classic data on AGN and stellar luminosity functions at high redshift z 1.5, to probe different stages in the coevolution of supermassive black holes (BHs) and host galaxies. The results of our analysis indicate the following scenario: (i) the star formation in the host galaxy proceeds within a heavily dust-enshrouded medium at an almost constant rate over a timescale 0.5 − 1 Gyr, and then abruptly declines due to quasar feedback; over the same timescale, (ii) part of the interstellar medium loses angular momentum, reaches the circum-nuclear regions at a rate proportional to the star formation and is temporarily stored into a massive reservoir/proto-torus wherefrom it can be promptly accreted; (iii) the BH grows by accretion in a self-regulated regime with radiative power that can slightly exceed the Eddington limit L/L Edd 4, particularly at the highest redshifts; (iv) for massive BHs the ensuing energy feedback at its maximum exceeds the stellar one and removes the interstellar gas, thus stopping the star formation and the fueling of the reservoir; (v) afterwards, if the latter has retained enough gas, a phase of supply-limited accretion follows exponentially declining with a timescale of about 2 e-folding times. We also discuss how the detailed properties and the specific evolution of the reservoir can be investigated via coordinated, high-resolution observations of starforming, strongly-lensed galaxies in the (sub-)mm band with ALMA and in the X-ray band with Chandra and the next generation X-ray instruments.

show abstract

“…In the true camp of co-formation reside one vote for accretion feeding both the bulge and the black hole at to 1.8 z p 2.8 ) and three for radiation drag as the dominant physics (Umemura 2001;Fabian et al 2002a;Kawakatu & Umemura 2002). The idea is that radiation drag by bulge stars takes angular momentum from gas and lets it accrete.…”

Section: The Pickle In the Middle: Black Hole-bulge Connectionsmentioning

confidence: 99%

Astrophysics in 2002

Trimble

Aschwanden

2003

PUBL ASTRON SOC PAC

View full text Add to dashboard Cite

ABSTRACT. This has been the Year of the Baryon. Some low temperature ones were seen at high redshift, some high temperature ones were seen at low redshift, and some cooling ones were (probably) reheated. Astronomers saw the back of the Sun (which is also made of baryons), a possible solution to the problem of ejection of material by Type II supernovae (in which neutrinos push out baryons), the production of R Coronae Borealis stars (previously-owned baryons), and perhaps found the missing satellite galaxies (whose failing is that they have no baryons). A few questions were left unanswered for next year, and an attempt is made to discuss these as well.

show abstract

Radiation drag driven mass accretion in a clumpy interstellar medium: implications for the supermassive black hole-to-bulge relation

Cited by 55 publications

References 40 publications

A Physical Model for the Coevolution of QSOs and Their Spheroidal Hosts

A Physical Model for the Coevolution of QSOs and Their Spheroidal Hosts

The Coevolution of Supermassive Black Holes and Massive Galaxies at High Redshift

Astrophysics in 2002

Contact Info

Product

Resources

About