Runaway Migration and the Formation of Hot Jupiters

By F. Masset, J. Papaloizou. 2003

279 citations recorded by the source corpus.

We evaluate the coorbital corotation torque on a migrating protoplanet. The coorbital torque is assumed to come from orbit crossing fluid elements that exchange angular momentum with the planet when they execute a U-turn at the end of horseshoe streamlines. When the planet migrates inward, the fluid elements of the inner disk undergo one such exchange as they pass to the outer disk. The angular momentum they gain is removed from the planet, and this corresponds to a negative contribution to the corotation torque, which scales with the drift rate. In addition, the material trapped in the coorbital region drifts radially with the planet, giving a positive contribution to the corotation torque, which also scales with the drift rate. These two contributions do not cancel out if the coorbital region is depleted, in which case there is a net corotation torque that scales with the drift rate and the mass deficit in the coorbital region and has the same sign as the drift rate. This leads to a positive feedback on the migrating planet. In particular, if the coorbital mass deficit is larger than the planet mass, the migration rate undergoes a runaway that can vary the protoplanet semimajor axis by 50% over a few tens of orbits. This can happen only if the planet mass is sufficient to create a dip or gap in its surrounding region and if the surrounding disk mass is larger than the planet mass. This typically corresponds to planet masses in the sub-Saturnian to Jovian mass range embedded in massive protoplanetary disks. Runaway migration is a good candidate to account for the orbital characteristics of close orbiting giant planets, most of which have sub-Jovian masses. These are known to cluster at short periods, whereas planets of greater than two Jovian masses are rare at short periods, indicating a different type of migration process operated for the two classes of object. Further, we show that in the runaway regime, migration can be directed outward, which makes this regime potentially rich in a variety of important effects in shaping a planetary system during the last stages of its formation.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/825f065c159549463d9cb93d01fa1117ecc17471

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Citations in the corpus

THE RUNTS OF THE LITTER: WHY PLANETS FORMED THROUGH GRAVITATIONAL INSTABILITY CAN ONLY BE FAILED BINARY STARS (2009, background): “…the core of a giant planet could be scattered outward by a planet, or migrate outward before accreting its gas envelope, either by interactions with the gas disk (Type III migration; e.g. Masset & Papaloizou 2003) or with planetesimals embedded in the gas (Capobianco, Duncan, & Levison, in prep).”
Radial Migration of Gap-opening Planets in Protoplanetary Disks. I. The Case of a Single Planet (2018, methodology): “When the planet forms a relatively shallow gap, the very fast typeIII migration can occur (Masset & Papaloizou 2003).”
The dynamics of Jupiter and Saturn in the gaseous protoplanetary disk (2007, background): “The migration of Saturn accelerates exponentially, in a runaway—also called Type III—regime (Masset and Papaloizou, 2003) that is well fitted by an exponential curve up to t ∼ 100.”
Origin and evolution of the atmospheres of early Venus, Earth and Mars (2018, methodology): “After the accretion of gas, Saturn migrated also inward but faster than Jupiter (e.g., Masset and Papaloizou 2003) and entered into a 2:3 mean motion resonance with Jupiter (Masset and Snellgrove 2001; Morbidelli and Crida 2007; Pierens and Nelson 2008).”
A torque formula for non-isothermal type I planetary migration – I. Unsaturated horseshoe drag (2009, background): “This radial flow of gas can be due to the migration of the planet itself, resulting in a positive feedback with the possibility of a runaway process (Masset & Papaloizou 2003), with migration time-scales of the order of a few tens of dynamical time-scales.”
Secular Dynamics in Hierarchical Three-Body Systems (2011, background): “If these planets migrated in from much larger distances through their interaction with the protoplanetary disk (Lin and Papaloizou 1986; Masset and Papaloizou 2003), their orbits should have low eccentricities and inclinations(4).”
TRANSITIONAL AND PRE-TRANSITIONAL DISKS: GAP OPENING BY MULTIPLE PLANETS? (2010, background): “…our simulations with relatively low planet masses (details are given later in this section), and the fact that planets grow slowly if f = 100 means that during our simulations rapid type I and type III migration are likely to dominate the evolution of the planet orbits (Masset and Papaloizou 2003).”
On the Migration of Protogiant Solid Cores (2006, methodology): “…have same dependency on the disk and planet parameters, and although the horseshoe drag may result in a very effective concept for some aspects of planetary migration related to coorbital material (Masset & Papaloizou 2003), there is no reason why these two quantities should be exactly the same.”
The Evolution of Gravitationally Unstable Protoplanetary Disks: Fragmentation and Possible Giant Planet Formation (2003, background): “…reversed because of either corotational or Lindblad torques once more realistic disks with profiles that are not simple power laws are considered (Masset & Papaloizou 2003; P. Artymowicz & W. Peplinski 2004, in preparation), but the mass doubling time of a Jupiter-sized 1 Institute of…”
Halting type I planet migration in non-isothermal disks (2006, background): “However, when the disk is massive enough, the planet enters a new migration mode that can be very fast and that relies on dynamical corotation torques (Masset & Papaloizou 2003; Artymowicz 2004).”
On the width and shape of gaps in protoplanetary disks (2005, background): “Type III (or runaway) migration corresponds to planets with intermediate mass, which do not open a clear gap, but only form a dip around their orbits in the gas surface density profile; under some conditions, their migration drift rate can grow exponentially, in a runaway process (Masset and Papaloi”
Planet formation and migration (2005, background): “D’Angelo et al (2005) have recently studied coorbital torques acting on a Saturn mass planet in a massive disk under a similar set up to Masset & Papaloizou (2003).”
The Eccentric Kozai-Lidov Effect and Its Applications (2016, background): “In the first channel, planets form in the disk, and in some cases, angular momentum exchange between the planets and the protoplanetary disk can produce inward migration (e.g., Lin and Papaloizou 1986; Masset and Papaloizou 2003).”
A torque formula for non-isothermal Type I planetary migration – II. Effects of diffusion (2010, background): “If the relative radial speed of the planet with respect to the gas is large enough, the streamline topology will be modified, leading to a flow structure similar to that encountered in Type III migration (Masset & Papaloizou 2003; Pepliński et al. 2008).”
Disk Surface Density Transitions as Protoplanet Traps (2006, background): “The edges of dead zones are thought, in the totally different context of runaway or type III migration (Masset & Papaloizou 2003), to be able to halt or reverse a runaway episode (Artymowicz 2004).”
Rapid inward migration of planets formed by gravitational instability (2011, background): “In massive (Q & 1) laminar discs with moderate viscosity (α is a few ×10−3), runaway migration is particularly relevant for planets with q ∼ h3p (Masset & Papaloizou 2003), like the planets considered in our study.”
ON THE FORMATION OF HOT JUPITERS IN STELLAR BINARIES (2012, background): “If these planets migrated in from much larger distances through their interaction with the protoplanetary disk (Lin & Papaloizou 1986; Masset & Papaloizou 2003), their orbits should have low eccentricities and inclinations (but see Lai et al. 2010; Thies et al. 2011).”