Hot Jupiters in Binary Star Systems

By Yanqin Wu, N. Murray, J. Ramsahai. 2007

160 citations recorded by the source corpus.

Radial velocity surveys find Jupiter-mass planets with semimajor axes a less than 0.1 AU around ~1% of solar-type stars; counting planets with a as large as 5 AU, the fraction of stars having planets reaches ~10% (as found by Marcy et al. and Butler et al.). An examination of the distribution of semimajor axes shows that there is a clear excess of planets with orbital periods around 3 or 4 days, corresponding to a ≈ 0.03 AU, with a sharp cutoff at shorter periods (see Fig. 1). It is believed that Jupiter-mass planets form at large distances from their parent stars; some fraction then migrates in to produce the short-period objects. We argue that a significant fraction of the hot Jupiters (a < 0.1 AU) may arise in binary star systems in which the orbit of the binary is highly inclined to the orbit of the planet. Mutual torques between the two orbits drive down the minimum separation or periapsis rp between the planet and its host star (the Kozai mechanism). This periapsis collapse is halted when tidal friction on the planet circularizes the orbit faster than Kozai torque can excite it. The same friction then circularizes the planet orbit, producing hot Jupiters with the peak of the semimajor axis distribution lying around 3 days. For the observed distributions of binary separation, eccentricity, and mass ratio, roughly 2.5% of planets with initial semimajor axis ap ≈ 5 AU will migrate to within 0.1 AU of their parent star. Kozai migration could account for 10% or more of the observed hot Jupiters.

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

View Paper: https://www.semanticscholar.org/paper/f4f3fd7c68884886b59d6c04b6d5fea43abd5f0c

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In Astronomy and Astrophysics

1. S. Naoz
2. B. Kocsis
3. F. Antonini
4. F. Rasio
5. Joseph M. Antognini
6. Y. Lithwick
7. J. Winn
8. Yanqin Wu

In Instrumentation

1. S. Naoz
2. F. Rasio
3. Y. Lithwick
4. F. Antonini
5. B. Kocsis
6. Joseph M. Antognini
7. T. Thompson
8. Yanqin Wu

In Statistical and Nonlinear Physics

1. Y. Lithwick
2. Yanqin Wu
3. S. Naoz
4. J. Winn
5. F. Rasio
6. W. Farr
7. Joseph M. Antognini
8. T. Thompson

Citations in the corpus

• EXOPLANETARY SPIN–ORBIT ALIGNMENT: RESULTS FROM THE ENSEMBLE OF ROSSITER–MCLAUGHLIN OBSERVATIONS (2009, background): “…occasionally large misalignments (Ford et al. 2001; Yu & Tremaine 2001; Papaloizou & Terquem 2001; Terquem & Papaloizou 2002; Marzari & Weidenschilling 2002; Thommes & Lissauer 2003; Wu et al. 2007; Fabrycky & Tremaine 2007; Chatterjee et al. 2008; Jurić & Tremaine 2008; Nagasawa et al. 2008).”
• Timescales of Kozai-Lidov oscillations at quadrupole and octupole order in the test particle limit (2015, background): “KL oscillations have been invoked in many contexts to explain a wide variety of phenomena such as the formation of hot Jupiters (Wu & Murray 2003; Wu et al. 2007; Fabrycky & Tremaine 2007; Naoz et al. 2011, 2012; Petrovich 2015), the formation of blue stragglers (Perets & Fabrycky 2009; Naoz &…”
• Rapid Eccentricity Oscillations and the Mergers of Compact Objects in Hierarchical Triples (2013, background): “The formation of hot Jupiters is a long-standing problem in the theory of planet formation and Kozai-Lidov cycles have been proposed as a mechanism to drive planets formed far from the host star into tight orbits (Wu et al. 2007).”
• SECULAR EVOLUTION OF COMPACT BINARIES NEAR MASSIVE BLACK HOLES: GRAVITATIONAL WAVE SOURCES AND OTHER EXOTICA (2012, result): “The oscillations in eccentricity and inclination observed in the computed orbits are reminiscent of the “Kozai cycles” generally discussed in the context of hierarchical triple systems (e.g. Harrington 1968; Wu et al. 2007; Naoz et al. 2011a; Prodan & Murray 2011).”
• SOAR TESS Survey. I. Sculpting of TESS Planetary Systems by Stellar Companions (2019, background): “…similar to the majority of planets detected by Kepler, and many large planets, 12 The Astronomical Journal, 159:19 (24pp), 2020 January Ziegler et al. similar to the extensively studied population of hot Jupiters (e.g., Wu et al. 2007; Knutson et al. 2014; Evans et al. 2016; Ngo et al. 2016).”
• A STELLAR-MASS-DEPENDENT DROP IN PLANET OCCURRENCE RATES (2014, background): “However, we note that the power-law index for tidal circularization after Kozai interactions with a binary companion (3/13, Wu et al. 2007), is the same as that for secular interaction in multi-planet systems (Table 2).”
• TIDAL EVOLUTION OF CLOSE-IN PLANETS (2010, methodology): “They also derived the stellar obliquity distribution by assuming an isotropic distribution of the stellar spin with respect to the line of sight, and found that the distribution closely matches that expected from the Kozai migration scenario (Fabrycky & Tremaine 2007; Wu et al. 2007).”
• 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).”
• SECULAR CHAOS AND THE PRODUCTION OF HOT JUPITERS (2010, background): “Kozai migration, in contrast, has no mass preferences (Wu et al. 2007).”
• ON THE FORMATION OF HOT JUPITERS IN STELLAR BINARIES (2012, methodology): “An alternative scenario that can account for the retrograde orbits involves the secular interaction between a planet and a binary stellar companion (Wu & Murray 2003; Fabrycky & Tremaine 2007; Wu et al. 2007; Takeda et al. 2008; Correia et al. 2011).”
• The Eccentric Kozai-Lidov Effect and Its Applications (2016, background): “An important outcome from these calculations was the prediction of retrograde Hot Jupiters (i.e., obliquities larger than 90◦) (Fabrycky and Tremaine 2007; Wu et al. 2007).”
• RESONANT POST-NEWTONIAN ECCENTRICITY EXCITATION IN HIERARCHICAL THREE-BODY SYSTEMS (2012, background): “…2007; Perets & Fabrycky 2009; Thompson 2010; Naoz et al. 2013; Prodan & Murray 2012; Sharpee & Thompson 2012) and extrasolar planetary systems with an additional distant stellar companion (e.g., Holman et al. 1997; Fabrycky & Tremaine 2007; Wu et al. 2007; Takeda et al. 2008; Naoz et al. 2012).”
• Secular Dynamics in Hierarchical Three-Body Systems (2011, methodology): “…1998; Kinoshita and Nakai 1999; Eggleton and Kiseleva-Eggleton 2001; Wu and Murray 2003; Valtonen and Karttunen 2006; Fabrycky and Tremaine 2007; Wu et al. 2007; Zdziarski et al. 2007; Perets and Fabrycky 2009), the assumption that H1 = const (i.e. the TPQ approximation) was built into the…”