Dynamics of Protoplanetary Disks

By Philip Armitage. 2010

438 citations recorded by the source corpus.

Protoplanetary disks are quasi-steady structures whose evolution and dispersal determine the environment for planet formation. I review the theory of protoplanetary disk evolution and its connection to observations. Substantial progress has been made in elucidating the physics of potential angular momentum transport processes—including self-gravity, magnetorotational instability, baroclinic instabilities, and magnetic braking—and in developing testable models for disk dispersal via photoevaporation. The relative importance of these processes depends upon the initial mass, size, and magnetization of the disk, and subsequently on its opacity, ionization state, and external irradiation. Disk dynamics is therefore coupled to star formation, pre-main-sequence stellar evolution, and dust coagulation during the early stages of planet formation and may vary dramatically from star to star. The importance of validating theoretical models is emphasized, with the key observations being those that probe disk structure...

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/8d7bf31cbb5a343bca6c8cce383b2157eeac78dc

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Citations in the corpus

Turbulence in the TW Hya Disk (2018, background): “The accretion rate through the disk is related to the surface density and α through: α = ṀΩ 3πΣc2s (1 − √ rin/r), (8) where Ṁ is the accretion rate, Ω is the Keplerian orbital frequency, Σ is the surface density, cs is the local sound speed, and rin is the inner radius of the disk (Armitage 2011).”
Astrophysics with Extraterrestrial Materials (2016, background): “Internal processes that might drive disk evolution include magnetorotational instability (MRI) (Balbus & Hawley 1991) and gravitational torques, each of which may operate in protoplanetary disks so long as certain conditions are met (Armitage 2011, Bai 2011, Bai & Stone 2013).”
On the theory of disc photoevaporation (2011, background): “This result raises the intriguing possibility that what determines the evolution of a disc (and presumably its ability to form planets) is the star’s intrinsic X-ray luminosity, rather than any variations in initial conditions when the star/disc system was created (Armitage 2011).”
Ice Condensation as a Planet Formation Mechanism (2013, background): “Seen over the life time of the disc this is not true, as the ice line probably moves both in a systematic way over long time scales and due to shorter heating events (Armitage, 2011).”
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).”
Debris disks as signposts of terrestrial planet formation (2011, background): “In particular, planetesimal formation is poorly understood (for a review, see Chiang & Youdin 2010), and may be coupled to the level of intrinsic turbulence within the gaseous disk, which probably varies with radius (Gammie 1996; Armitage 2011).”
WEAK TURBULENCE IN THE HD 163296 PROTOPLANETARY DISK REVEALED BY ALMA CO OBSERVATIONS (2015, background): “Gravito-turbulence has been suggested as an alternative to MRI as the driver of turbulence within the disk (Armitage 2011), although as with MRI the predicted magnitude is still larger than our upper limits.”
Observational Signatures of Planets in Protoplanetary Disks I: Gaps Opened by Single and Multiple Young Planets in Disks (2014, background): “These disks are considered to be the birth place of planets (Armitage 2011).”
Our astrochemical heritage (2012, methodology): “on the chemical evolution (see [18] and [463] for comprehensive reviews on the physical characteristics and evolution of protoplanetary disks).”
Planet-Disk Interaction and Orbital Evolution (2012, background): “The structure and dynamics of these disks are clearly relevant for understanding planet formation, and we refer the interested reader to three recent reviews that discuss the theory and observations of protoplanetary disks (Dullemond & Monnier, 2010; Armitage, 2011; Williams & Cieza, 2011).”
Survival of molecular gas in cavities of transition disks - I. CO (2013, background): “A detailed understanding of the evolution and dissipation of protoplanetary disks is thus crucial to constrain theories of planet formation (see Armitage 2011, for a recent review).”
KEPLER PLANETS: A TALE OF EVAPORATION (2013, background): “We could of course parametrise the initial entropy in terms of some other variables; however, the initial cooling time is perhaps the most interesting as this be compared to protoplanetary discs lifetimes ∼3 Myr (e.g. Haisch et al. 2001; Hernández et al. 2007; Owen et al. 2011; Armitage 2011).”
IN SITU FORMATION AND DYNAMICAL EVOLUTION OF HOT JUPITER SYSTEMS (2015, background): “3 Strictly speaking, the assumption of spherical symmetry inherent to the employed model is only well justified as long as the Hill radius does not exceed the disk scale height (i.e. rH/a < h/a ∼ 0.05 − 0.1; Armitage 2011).”
THE MASS–METALLICITY RELATION FOR GIANT PLANETS (2015, background): “Assuming that gas accretion through the gap becomes inefficient for Δ/RH=fS∼5 (Lissauer et al. 2009; Kratter et al. 2010), a planet mass Mp set by gap truncation implies the disk viscosity parameter (Shakura & Sunyaev 1973; Armitage 2011) ( ) * a p = - ⎜ ⎟⎛⎝ ⎞ ⎠ f f M M H r .”
Linear and non-linear evolution of the vertical shear instability in accretion discs (2012, background): “It is also likely that the MRI is quenched by ambipolar diffusion in the very outermost regions of protostellar discs (Armitage 2011), so these may also provide low-density, magnetically inactive regions where the vertical shear instability can operate.”
Accretion and differentiation of the terrestrial planets with implications for the compositions of early-formed Solar System bodies and accretion of water (2014, background): “Simple model temperatures and pressures at the midplane of the solar accretion disk predict that the snow line migrated inward from about 5 AU to 2 AU as the rate of accretion of the protoplanetary disk onto the central star decreased from 10-7 Me yr-1 to 10-8 Me yr-1 (Armitage, 2011).”