Planet Migration and Binary Companions: The Case of HD 80606b

By Yanqin WuNorm Murray. 2003

534 citations recorded by the source corpus.

The exosolar planet HD 80606b has a highly eccentric (e = 0.93) and tight (a = 0.47 AU) orbit. We study how it might arrive at such an orbit and how it has avoided being tidally circularized until now. The presence of a stellar companion to the host star suggests the possibility that the Kozai mechanism and tidal dissipation combined to draw the planet inward well after it formed: Kozai oscillations produce periods of extreme eccentricity in the planet orbit, and the tidal dissipation that occurs during these periods of small pericenter distances leads to gradual orbital decay. We call this migration mechanism the "Kozai migration." It requires that the initial planet orbit be highly inclined relative to the binary orbit. For a companion at 1000 AU and an initial planet orbit at 5 AU, the minimum relative inclination required is ~85°. We discuss the efficiency of tidal dissipation inferred from the observations of exoplanets. Moreover, we investigate possible explanations for the velocity residual (after the motion induced by the planet is removed) observed on the host star: a second planet in the system is excluded over a large extent of semimajor axis space if Kozai migration is to work, and the tide raised on the star by HD 80606b is likely too small in amplitude. Last, we discuss the relevance of Kozai migration for other planetary systems.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/7cb3c07703dceb918ad669aec0da5e1a1e2d9f6f

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In Astronomy and Astrophysics

1. Jon Fortney
2. D. Charbonneau
3. J. Winn
4. J. Johnson
5. C. Mordasini
6. M. Perryman
7. N. Madhusudhan
8. J. Owen

In Instrumentation

1. D. Charbonneau
2. Jon Fortney
3. Timothy Morton
4. J. Johnson
5. J. Winn
6. Andrew W. Howard
7. J. Owen
8. G. Marcy

In Statistical and Nonlinear Physics

1. Jon Fortney
2. Y. Lithwick
3. J. Owen
4. D. Charbonneau
5. Timothy Morton
6. Yanqin Wu
7. C. Mordasini
8. S. Naoz

Citations in the corpus

• PLANETARY POPULATION SYNTHESIS COUPLED WITH ATMOSPHERIC ESCAPE: A STATISTICAL VIEW OF EVAPORATION (2014, background): “A close-in planet may also be formed through Kozai migration with tidal circularization (Wu & Murray 2003; Fabrycky & Tremaine 2007), but this process can take considerably longer, and the intense atmospheric evaporation stage may have passed.”
• TESTING IN SITU ASSEMBLY WITH THE KEPLER PLANET CANDIDATE SAMPLE (2013, background): “…therein) has cast some doubt on the applicability of this model to at least some of the observed systems, reviving interest in such mechanisms as planetary scattering (Rasio & Ford 1996; Nagasawa & Ida 2011) or Kozai migration (Wu & Murray 2003; Fabrycky & Tremaine 2007; Naoz et al. 2011).”
• Planet-Disk Interaction and Orbital Evolution (2012, background): “…the best contender for explaining the large eccentricities of extrasolar planets (Terquem & Papaloizou, 2002; Jurić & Tremaine, 2008; Chatterjee et al., 2008), and the Kozai mechanism drives high eccentricities through secular interaction with a highly inclined companion (Wu & Murray, 2003).”
• Protoplanetary disk lifetimes vs stellar mass and possible implications for giant planet populations (2015, background): “Other migration processes such as planet-planet scattering, Kozai resonances, or similar dynamic mechanisms (e.g. Kozai 1962; Wu & Murray 2003; Naoz et al. 2011) are likely responsible for the fraction of hot Jupiters whose spin is found to be misaligned with their planet-star orbits (Triaud et al.…”
• Rapid Eccentricity Oscillations and the Mergers of Compact Objects in Hierarchical Triples (2013, background): “…in the Solar System (Kozai 1962), the orbits of artificial satellites around planets in the Solar System (Lidov 1962), as a formation channel for hot Jupiters (e.g., Wu & Murray 2003; Fabrycky & Tremaine 2007; Wu et al. 2007), and as a formation channel for blue stragglers (Perets & Fabrycky 2009).”
• The California-Kepler Survey. IV. Metal-rich Stars Host a Greater Diversity of Planets (2017, background): “A non-exhaustive list of theories includes star-planet Kozai (e.g. Wu & Murray 2003), planetplanet Kozai (e.g. Naoz et al. 2011), smooth disk-driven Type-I migration (e.g. Ida & Lin 2008), high eccentricity migration, and in situ formation (e.g. Batygin et al. 2016).”
• The M-dwarfs in Multiples (MinMs) survey – I. Stellar multiplicity among low-mass stars within 15 pc (2015, background): “There are indications that some exoplanet systems have been impacted by this dynamical effect (e.g. Wu & Murray 2003), and simulations of early dynamical interactions in star-forming regions have shown that the Kozai mechanism could be induced in up to 20 per cent of field binaries (Parker &…”
• The Eccentric Kozai-Lidov Effect and Its Applications (2016, background): “ai-Lidov mechanism (in the framework of the TPQ approximation). They also showed that the planet spends about ˘35% of its lifetime in a high eccentric orbit e>0:6. In subsequent nominal studies by Wu and Murray (2003), Wu et al. (2007) and Fabrycky and Tremaine (2007) the consequences of the TPQ ”
• ACCELERATING COMPACT OBJECT MERGERS IN TRIPLE SYSTEMS WITH THE KOZAI RESONANCE: A MECHANISM FOR “PROMPT” TYPE Ia SUPERNOVAE, GAMMA-RAY BURSTS, AND OTHER EXOTICA (2010, background): “…action of tidal friction and Kozai oscillations on the period distrbution of solar-type binaries in triple systems has been considered in detail by FT07 (see also Mazeh & Shaham 1979; Kiseleva et al. 1998; Eggleton & Kiseleva-Eggleton 2001; Wu & Murray 2003; Wu et al. 2007; Perets & Fabrycky 2009).”
• INTERNAL GRAVITY WAVES IN MASSIVE STARS: ANGULAR MOMENTUM TRANSPORT (2013, background): “Some of those may indeed be due to dynamical effects, such as the Kozai mechanism (Wu & Murray 2003).”
• FRIENDS OF HOT JUPITERS. I. A RADIAL VELOCITY SEARCH FOR MASSIVE, LONG-PERIOD COMPANIONS TO CLOSE-IN GAS GIANT PLANETS (2013, background): “There are currently two systems (HD 80606b and 16 Cyg Bb) where there is clear evidence for orbital evolution of an eccentric Jovian-mass exoplanet due to interactions with a distant stellar companion (Holman et al. 1997; Wu & Murray 2003).”
• Unresolved stellar companions with Gaia DR2 astrometry (2020, background): “…distances either through angular momentum loss inside a remnant circumstellar disc (e.g. Goldreich & Tremaine 1980; Lin & Papaloizou 1986) or via interactions with other companions of their hosts, perhaps through the Kozai–Lidov mechanism (e.g. Wu & Murray 2003; Fabrycky & Tremaine 2007).”
• On the tidal evolution of Hot Jupiters on inclined orbits (2009, background): “This is Kozai migration (Wu & Murray 2003).”
• SECULAR CHAOS AND THE PRODUCTION OF HOT JUPITERS (2010, background): “First proposed by Wu & Murray (2003), it asserts that a highly inclined companion star can induce Kozai oscillations (Kozai 1962; Eggleton & Kiseleva-Eggleton 2001) in the planet, gradually exciting the planet to a high enough eccentricity that it approaches the central star, whereupon tidal…”
• Formation of Hot Planets by a Combination of Planet Scattering, Tidal Circularization, and the Kozai Mechanism (2008, background): “Wu (2003) and Wu & Murray (2003) also pointed out the migration due to a coupled effect of the Kozai mechanism and tidal circularization for a planet in a binary system and called it ‘‘Kozai migration.’’”
• Tidal dissipation in planet-hosting stars: damping of spin-orbit misalignment and survival of hot Jupiters (2011, background): “…& Tremaine 2008) and more importantly, through secular interactions between multiple planets or Kozai effect induced by a distant companion (e.g., Wu & Murray 2003; Fabrycky & Tremaine 2007; Nagasawa et al. 2008; Naoz et al. 2011a,b; Wu & Lithwick 2011; Katz et al. 2011), although other…”
• THE ECCENTRIC KOZAI MECHANISM FOR A TEST PARTICLE (2011, background): “But when Jupiter’s orbit is eccentric, the dynamics can no longer be solved analytically.”
• MULTIPLE-PLANET SCATTERING AND THE ORIGIN OF HOT JUPITERS (2011, background): “Indeed we found no clear examples of the standard Kozai migration (Wu & Murray 2003).”
• ON THE FORMATION OF HOT JUPITERS IN STELLAR BINARIES (2012, background): “Many theoretical studies have investigated the role of secular perturbations in triple systems (Holman et al. 1997; Wu & Murray 2003; Takeda & Rasio 2005; Fabrycky & Tremaine 2007; Wu et al. 2007; Takeda et al. 2008; Correia et al. 2011; Naoz et al. 1 Harvard Smithsonian Center for Astrophysics,…”