Enhanced Angular Momentum Transport in Accretion Disks

By Steven Balbus. 2003

383 citations recorded by the source corpus.

▪ Abstract The status of our current understanding of angular momentum transport in accretion disks is reviewed. The last decade has seen a dramatic increase both in the recognition of key physical...

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/86485706a7c12cd37aca466dbdcd580df77e9044

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Citations in the corpus

STRUCTURE AND EVOLUTION OF PRE-MAIN-SEQUENCE CIRCUMSTELLAR DISKS (2009, background): “Numerical simulations of keplerian disk affected by MRI suggest that α can range from 0.005 to 0.6 (see, e.g., the review of Balbus 2003).”
Polarimetry of near-infrared flares from Sagittarius A* (2006, background): “However, magnetic field configurations in accretion flows and (temporal) disks may have a strong turbulent component as well (Shakura & Sunyaev 1973; Duschl et al. 1991; Balbus 2003).”
EFFECT OF AMBIPOLAR DIFFUSION ON THE NONLINEAR EVOLUTION OF MAGNETOROTATIONAL INSTABILITY IN WEAKLY IONIZED DISKS (2011, background): “Such oscillations are likely to associate with linear modes in the shearing sheet with the origin of acoustic and/or nearly incompressible inertia waves (Balbus 2003).”
CIRCUMVENTING THE RADIATION PRESSURE BARRIER IN THE FORMATION OF MASSIVE STARS VIA DISK ACCRETION (2010, background): “…pressure feedback: developing radiation hydrodynamical (Klahr & Bodenheimer 2003), magnetorotational (Balbus & Hawley 1991; Hawley & Balbus 1991; Balbus 2003), and self-gravitating instabilities (Yang et al. 1991; Laughlin & Bodenheimer 1994; Bodenheimer 1995) in the accretion disk will…”
The subcritical baroclinic instability in local accretion disc models (2009, background): “The reader may consult Hawley et al. (1995), Balbus (2003) and Regev & Umurhan (2008) for an extensive discussion of the properties and limitations of this model.”
What drives the growth of black holes (2011, background): “Magnetic fields are likely to dominate viscosity and the transport of angular momentum in accretion discs, as suggested by numerical simulations of Magneto-Rotational Instability (MRI; e.g., Balbus & Hawley 1991, 1998; Balbus 2003).”
Supercritical Accretion Flows around Black Holes: Two-dimensional, Radiation Pressure-dominated Disks with Photon Trapping (2005, methodology): “More importantly, we need coupled MHD and RHD simulations, since the source of disk viscosity is likely to be of magnetic origins (Hawley, Balbus, & Stone 2001; Machida, Matsumoto, & Mineshige 2001; Balbus 2003 for a review).”
Toward Understanding Massive Star Formation (2007, background): “Efficient angular momentum transfer could result from weak magnetic fields in the disk (Balbus & Hawley 1991, Hawley & Balbus 1991, Balbus 2003), from turbulence and/or spiral density waves (Bodenheimer 1995) excited by gravitational instabilities in nonmagnetized (Laughlin & Bodenheimer 1994) or…”
Theory of Star Formation (2007, background): “Much effort has been devoted to exploring the MRI as a basic mechanism driving accretion in a variety of systems; Balbus & Hawley (1998) and Balbus (2003) summarize many of the these developments.”
Three-dimensional GRMHD Simulations of Neutrino-cooled Accretion Disks from Neutron Star Mergers (2017, background): “Turbulence is thought to be generated in this context by the MRI, which refers to certain exponentially growing modes that can develop in differentially rotating magnetized fluids (e.g., Velikhov 1959; Chandrasekhar 1960; Balbus & Hawley 1991, 1998; Balbus 2003; Armitage 2011).”
THREE-DIMENSIONAL SIMULATION OF MASSIVE STAR FORMATION IN THE DISK ACCRETION SCENARIO (2011, background): “A more recent review on angular momentum transport in accretion disks is presented by Balbus (2003) and an overview of standard accretion disk theory in general is given in Lodato (2008).”
“Propeller” Regime of Disk Accretion to Rapidly Rotating Stars (2006, neutral): “The value of αv is in the rough interval 3× 10−3− 0.4 (Balbus 2003).”
On the relevance of subcritical hydrodynamic turbulence to accretion disk transport (2005, neutral): “…important example of supercritical transition is provided by the magneto-rotational instability (MRI) which has been extensively studied following the pioneering work of Balbus, Hawley and their collaborators (Balbus & Hawley 1991; Hawley et al. 1995; see Balbus 2003, for a recent review).”
THE LONG-TERM EVOLUTION OF DOUBLE WHITE DWARF MERGERS (2011, background): “In particular, if magneticallygoverned processes such as the magnetorotational instability (Balbus & Hawley 1991; Hawley & Balbus 1991; Balbus 2003) and the Tayler-Spruit dynamo (Tayler 1973; Spruit 1999, 2002) operate efficiently, angular momentum will be redistributed throughout the remnant much…”
Broad Iron-Kα Emission Lines as a Diagnostic of Black Hole Spin (2007, background): “From the body of literature on MRI driven turbulence (e.g., see Balbus 2003), we expect the final turbulent state to be independent of most aspects of the initial field configuration (e.g., see the study of Hawley 2000).”
Characterizing the gravitational instability in cooling accretion discs (2008, background): “In the context of gaseous (accretion) discs, qualitatively similar (but rather more involved) analyses have been present d in Balbus & Papaloizou (1999) and Balbus (2003).”
Paleomagnetic Records of Meteorites and Early Planetesimal Differentiation (2010, background): “The inner ionized region of the protoplanetary disk is thought to have been unstable to the magnetorotational instability (Balbus 2003, 2009), which likely generated spatially complex fields of up to ∼100 µT (Sano et al. 2004; Johansen 2009).”
IMPLEMENTATION OF THE SHEARING BOX APPROXIMATION IN ATHENA (2010, background): “Nevertheless it has provided a useful laboratory for the study of important questions related to the local dynamics of accretion disks (Balbus 2003).”
Super-Eddington Accretion Disks around Supermassive Black Holes (2017, neutral): “…on the linear analysis of density waves, the amount of Reynolds stress generated by the density waves is proportional to the turbulent radial kinetic energy as (Balbus 2003, Equation 43) 〈〈δρvrδvφ 〉〉= m rkr ( 1− κ 2 m2 (Ω− Ωp)2 ) 〈〈ρδv2r 〉〉 = cr,s r √ (Ω− Ωp)2 − κ2/m2 (Ω− Ωp)2 〈〈ρδv2r 〉〉.”