Three-dimensional Interaction between a Planet and an Isothermal Gaseous Disk. II. Eccentricity Waves and Bending Waves

By Hidekazu Tanaka, W. Ward. 2004

296 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/d453e93da403cb41e6f89b61ca76a591f8c0424b

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

OVERSTABLE LIBRATIONS CAN ACCOUNT FOR THE PAUCITY OF MEAN MOTION RESONANCES AMONG EXOPLANET PAIRS (2013, methodology): “For example, the plant-disk model investigated by Tanaka & Ward (2004) yields p ∼ 1.3.”
Dynamics of the Giant Planets of the Solar System in the Gaseous Protoplanetary Disk and Their Relationship to the Current Orbital Architecture (2007, background): “lanar in our N-body simulations. We do not think that this is a signi???cant limitation because it is well known that gas disks very e???ectively damp planetary inclinations (Lubow and Ogilvie, 2001; Tanaka and Ward, 2004) and we see no way to e???ectively excite them again. Planetary inclinations c”
Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion (2017, methodology): “Gravitational interactions with the disk damp the cores’ eccentricities and inclinations (Papaloizou and Larwood, 2000; Tanaka and Ward, 2004), although this is only important for core-core interactions (i.”
Planet-Disk Interaction and Orbital Evolution (2012, background): “Linear analysis for low-mass planets indicate rapid exponential damping of eccentricity, dep/dt ∝ −ep, on timescales of τecc ≈ (H/r)2τmig for small initial eccentricities (Tanaka & Ward, 2004), primarily because of the damping provided by the coorbital Lindblad resonances.”
TEN NEW AND UPDATED MULTIPLANET SYSTEMS AND A SURVEY OF EXOPLANETARY SYSTEMS (2008, background): “Thus it appears that short-period planets form farther out and migrate inwards to their final semimajor axis (Papaloizou 2005; Tanaka & Ward 2004; Trilling, Lunine, & Benz 2002).”
Breaking the chains: hot super-Earth systems from migration and disruption of compact resonant chains (2017, methodology): “…(Goldreich & Tremaine 1979, 1980; Lin & Papaloizou 1979, 1986; Ward 1986; Artymowicz 1993; Ward 1997; Tanaka, Takeuchi & Ward 2002; Sari & Goldreich 2004), as well as eccentricity and inclination damping of the planets’ orbit (Papaloizou & Larwood 2000; Goldreich & Sari 2003; Tanaka & Ward 2004).”
ZODIACAL EXOPLANETS IN TIME (ZEIT). III. A SHORT-PERIOD PLANET ORBITING A PRE-MAIN-SEQUENCE STAR IN THE UPPER SCORPIUS OB ASSOCIATION (2016, background): “This is expected for a young Neptunemass planet where recent interactions with the nascent disk have dampened eccentricity (e.g., Tanaka & Ward 2004; Cresswell et al. 2007).”
Planet formation and migration (2005, background): “…full linear analysis of the excited waves in two or three dimensions (see, for example, Korycansky & Pollack 1993, Tanaka et al 2002, Terquem 2003, Tanaka & Ward 2004) or by summing up the contribution of point like torques exerted at Lindblad and corotation resonances (see, for example,…”
Three-dimensional simulations of multiple protoplanets embedded in a protostellar disc (2008, methodology): “Our starting point is the formulae for damping rates obtained by Tanaka & Ward (2004) and the migration rates obtained by Tanaka et al. (2002), which we modify using multiplicative factors that account for changes in damping and migration rates due to planetary eccentricity and/or inclination.”
On the evolution of multiple protoplanets embedded in a protostellar disc (2006, methodology): “We thus adopt the formula obtained by Tanaka & Ward (2004) for the eccentricity evolution of low mass planets in 3D discs appropriate to small eccentricity.”
TOWARD A DETERMINISTIC MODEL OF PLANETARY FORMATION. VI. DYNAMICAL INTERACTION AND COAGULATION OF MULTIPLE ROCKY EMBRYOS AND SUPER-EARTH SYSTEMS AROUND SOLAR-TYPE STARS (2010, background): “In the linear calculations (Tanaka et al. 2002; Tanaka & Ward 2004), the timescale of the eccentric damping (τe) is shorter than that of type I migration (τmig) by a factor of ∼(cs/vK)2 ∼ O(10−3).”
Terrestrial Planet Formation. I. The Transition from Oligarchic Growth to Chaotic Growth (2005, background): “For a gaseous disk with the surface density of a minimum mass solar nebula, the circularization timescale for an oligarch is τc ∼ 0.1–0.2 Myr at 1 AU (Agnor & Ward 2002; Tanaka & Ward 2004).”
IN SITU FORMATION AND DYNAMICAL EVOLUTION OF HOT JUPITER SYSTEMS (2015, background): “…resonances among close-in sub-Jovian planets11 points to the fact that type-I migration (however it might proceed) does not ubiquitously drive planets into the magnetospheric cavity, as predicted within the framework of simplified isothermal calculations (e.g. Ward 1997; Tanaka et al. 2002).”
Spacing of Kepler Planets: Sculpting by Dynamical Instability (2015, background): “To put this timescale into context, the expected e-damping time from Type-I migration in a minimum mass solar nebula is τdamp ∼ 3 yrs (Tanaka & Ward 2004).”