Shrinking Binary and Planetary Orbits by Kozai Cycles with Tidal Friction

By D. Fabrycky, Scott Tremaine. 2007

1,107 citations recorded by the source corpus.

At least two arguments suggest that the orbits of a large fraction of binary stars and extrasolar planets shrank by 1-2 orders of magnitude after formation: (1) the physical radius of a star shrinks by a large factor from birth to the main sequence, yet many main-sequence stars have companions orbiting only a few stellar radii away, and (2) in current theories of planet formation, the region within ~0.1 AU of a protostar is too hot and rarefied for a Jupiter-mass planet to form, yet many "hot Jupiters" are observed at such distances. We investigate orbital shrinkage by the combined effects of secular perturbations from a distant companion star (Kozai oscillations) and tidal friction. We integrate the relevant equations of motion to predict the distribution of orbital elements produced by this process. Binary stars with orbital periods of 0.1-10 days, with a median of ~2 days, are produced from binaries with much longer periods (10 to ~105 days), consistent with observations indicating that most or all short-period binaries have distant companions (tertiaries). We also make two new testable predictions: (1) For periods between 3 and 10 days, the distribution of the mutual inclination between the inner binary and the tertiary orbit should peak strongly near 40° and 140°. (2) Extrasolar planets whose host stars have a distant binary companion may also undergo this process, in which case the orbit of the resulting hot Jupiter will typically be misaligned with the equator of its host star.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/1e8a07f67269496f2ab7708eaf808f7947ee2d21

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Citations in the corpus

THE ECCENTRIC KOZAI MECHANISM FOR A TEST PARTICLE (2011, background): “For example, in triple star systems, if the outer star is inclined it can force Kozai oscillations in the inner binary, increasing the inner binary’s eccentricity until tidal dissipation circularizes it into a very tight orbit (e.g., Eggleton & Kiseleva-Eggleton 2001; Fabrycky & Tremaine 2007).”
Evolution of spin direction of accreting magnetic protostars and spin-orbit misalignment in exoplanetary systems (2010, background): “…disc has dissipated to the present, involves dynamical gravitational interactions between multiple planets if they are produced in the ﬁrst stage in a suﬃciently close-packed conﬁguration (e.g., interactions with a distant planet or stellar companion (Wu & Murray 2003; Fabrycky & Tremaine 2007).”
FROM BINARIES TO MULTIPLES. I. DATA ON F AND G DWARFS WITHIN 67 pc OF THE SUN (2014, background): “Stellar hierarchies matter because they evolve differently from simple binaries, helping to form close binaries (Fabrycky & Tremaine 2007) and more exotic objects like blue stragglers (Peters & Fabrycky 2009).”
The GAPS Programme with HARPS-N at TNG - XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets (2017, neutral): “…(e.g. Chatterjee et al. 2008), Kozai-type perturbations induced by a distant stellar or planetary companion on a highly inclined orbit (e.g. Fabrycky & Tremaine 2007; Naoz et al. 2011), secular dynamics in multi-planet systems (e.g. Wu & Lithwick 2011; Hamers et al. 2017), or a combination…”
THE IMPACT OF STELLAR MULTIPLICITY ON PLANETARY SYSTEMS. I. THE RUINOUS INFLUENCE OF CLOSE BINARY COMPANIONS (2016, background): “…2006; Kratter & Perets 2012; Kaib et al. 2013), though dynamical interactions also have been suggested as a channel for producing the many giant planets discovered well inside the snow line (Kozai 1962; Fabrycky & Tremaine 2007; Winn et al. 2010; Naoz et al. 2012; but also Ngo et al. 2015).”
ORBITAL PHASE VARIATIONS OF THE ECCENTRIC GIANT PLANET HAT-P-2b (2013, background): “…distance, ac, of 10 to 40 AU from HAT-P-2b lends credence to the possibility that HAT-P-2b owes is current orbit to a history of Kozai cycling (Kozai 1962) combined with long-running orbital decay generated by tidal friction (Eggleton et al. 1998; Wu & Murray 2003; Fabrycky & Tremaine 2007).”
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).”
ECCENTRICITY FROM TRANSIT PHOTOMETRY: SMALL PLANETS IN KEPLER MULTI-PLANET SYSTEMS HAVE LOW ECCENTRICITIES (2015, background): “Planet-planet interactions have been brought forward as a mechanism to explain the observed eccentricities in massive planets (Fabrycky & Tremaine 2007; Chatterjee et al. 2008; Nagasawa et al. 2008; Ford & Rasio 2008; Jurić & Tremaine 2008).”
Secular Dynamics in Hierarchical Three-Body Systems (2011, methodology): “…al. 1998; Mikkola and Tanikawa 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…”
Photoevaporation and high-eccentricity migration created the sub-Jovian desert (2018, background): “…other planets or with a distant stellar companion, followed by tidal dissipation which circularises the planetâĂŹs orbit (e.g., Wu & Murray 2003; Fabrycky & Tremaine 2007; Nagasawa, Ida & Bessho 2008; Wu & Lithwick 2011; Beauge & Nesvorny 2012; Naoz et al. 2012; Petrovich 2015; Anderson,…”
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.”
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).”
FRIENDS OF HOT JUPITERS. I. A RADIAL VELOCITY SEARCH FOR MASSIVE, LONG-PERIOD COMPANIONS TO CLOSE-IN GAS GIANT PLANETS (2013, background): “…to this result, migration mechanisms involving multi-body interactions such as Kozai migration (e.g., Wu & Murray 2003; Malmberg et al. 2007; Fabrycky & Tremaine 2007; Naoz et al. 2012; Teyssandier et al. 2013b), which requires a distant stellar companion, planet-planet scattering (e.g.,…”
EVIDENCE OF POSSIBLE SPIN–ORBIT MISALIGNMENT ALONG THE LINE OF SIGHT IN TRANSITING EXOPLANET SYSTEMS (2010, methodology): “Using these parameters, I evolve the initial period given by the randomly selected mass and the initial period-mass relation described in Figure 2 to the randomly selected age of the system according to Equation 1.”
BLACK HOLE MERGERS AND BLUE STRAGGLERS FROM HIERARCHICAL TRIPLES FORMED IN GLOBULAR CLUSTERS (2015, background): “Lidov-Kozai (LK) oscillations are usually described as a secular phenomenon, occurring on timescales much longer than the orbital period of the outer binary orbit (e.g., Ford et al. 2004; Fabrycky & Tremaine 2007; Naoz et al. 2013).”
ZODIACAL EXOPLANETS IN TIME (ZEIT). III. A SHORT-PERIOD PLANET ORBITING A PRE-MAIN-SEQUENCE STAR IN THE UPPER SCORPIUS OB ASSOCIATION (2016, background): “…that it either migrated inwards via disk migration or formed in-situ, as planetstar and planet-planet interactions work on much longer timescales (Fabrycky & Tremaine 2007; Nagasawa et al. 2008), and the conditions for Kozai-Lidov evolution only begin after the disk dissipates (e.g., Martin et…”