NEW OBSERVATIONAL CONSTRAINTS ON THE υ ANDROMEDAE SYSTEM WITH DATA FROM THE<i>HUBBLE SPACE TELESCOPE</i>AND HOBBY-EBERLY TELESCOPE

McArthur, B.; Benedict, G. F.; Barnes, Rory; Martioli, E.; Korzennik, S. G.; Nelan, E.; Butler, R. Paul

doi:10.1088/0004-637x/715/2/1203

Cited by 155 publications

(159 citation statements)

References 82 publications

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“…• from each other (McArthur et al 2010). Similarly, the retrograde hot Jupiter in WASP-8b (Queloz et al 2011) is in a stellar system including an M-star companion at ∼600 AU.…”

Section: Stellar Obliquitymentioning

confidence: 91%

Secular Chaos and the Production of Hot Jupiters

Lithwick

2011

ApJ

390

356

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In a planetary system with two or more well-spaced, eccentric, inclined planets, secular interactions may lead to chaos. The innermost planet may gradually become very eccentric and/or inclined as a result of the secular degrees of freedom drifting toward equipartition of angular momentum deficit. Secular chaos is known to be responsible for the eventual destabilization of Mercury in our own solar system. Here we focus on systems with three giant planets. We characterize the secular chaos and demonstrate the criterion for it to occur, but leave a detailed understanding of secular chaos to a companion paper. After an extended period of eccentricity diffusion, the inner planet's pericenter can approach the star to within a few stellar radii. Strong tidal interactions and ensuing tidal dissipation extract orbital energy from the planet and pull it inward, creating a hot Jupiter. In contrast to other proposed channels for the production of hot Jupiters, such a scenario (which we term "secular migration") explains a range of observations: the pile-up of hot Jupiters at 3 day orbital periods, the fact that hot Jupiters are in general less massive than other radial velocity planets, that they may have misaligned inclinations with respect to stellar spin, and that they have few easily detectable companions (but may have giant companions in distant orbits). Secular migration can also explain close-in planets as low in mass as Neptune; and an aborted secular migration can explain the "warm Jupiters" at intermediate distances. In addition, the frequency of hot Jupiters formed via secular migration increases with stellar age. We further suggest that secular chaos may be responsible for the observed eccentricities of giant planets at larger distances and that these planets could exhibit significant spin-orbit misalignment.

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“…• from each other (McArthur et al 2010). Similarly, the retrograde hot Jupiter in WASP-8b (Queloz et al 2011) is in a stellar system including an M-star companion at ∼600 AU.…”

Section: Stellar Obliquitymentioning

confidence: 91%

Secular Chaos and the Production of Hot Jupiters

Lithwick

2011

ApJ

390

356

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“…Michtchenko et al 2006b, Libert & Henrard 2007, Libert & Tsiganis 2009a. A first observational confirmation (McArthur et al 2010) for the υ Andromedae system estimated the mutual inclination of the orbital planes of planets c and d of this system to ∼ 30 • .…”

Section: Introductionmentioning

confidence: 91%

Trapping in three-planet resonances during gas-driven migration

Libert

Tsiganis

2011

Celest Mech Dyn Astr

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We study the establishment of three-planet resonances -similar to the Laplace resonance in the Galilean satellites -and their effects on the mutual inclinations of the orbital planes of the planets, assuming that the latter undergo migration in a gaseous disc. In particular, we examine the resonance relations that occur, by varying the physical and initial orbital parameters of the planets (mass, initial semi-major axis and eccentricity) as well as the parameters of the migration forces (migration rate and eccentricity damping rate), which are modeled here through a simplified analytic prescription. We find that, in general, for planetary masses below 1.5 M J , multiple-planet resonances of the form n 3 :n 2 :n 1 =1:2:4 and 1:3:6 are established, as the inner planets, m 1 and m 2 , get trapped in a 1:2 resonance and the outer planet m 3 subsequently is captured in a 1:2 or 1:3 resonance with m 2 . For mild eccentricity damping, the resonance pumps the eccentricities of all planets on a relatively short time-scale, to the point where they enter an inclination-type resonance (as in Libert & Tsiganis 2011); then mutual inclinations can grow to ∼ 35 • , thus forming a "3-D system". On the other hand, we find that trapping of m 2 in a 2:3 resonance with m 1 occurs very rarely, for the range of masses used here, so only two cases of capture in a respective three-planet resonance were found. Our results suggest that trapping in a three-planet resonance can be common in exoplanetary systems, provided that the planets are not very massive. Inclination pumping could then occur relatively fast, provided that eccentricity damping is not very efficient so that at least one of the inner planets acquires an orbital eccentricity higher than e = 0.3.

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“…There are triple stars with nearly perpendicular orbits, like Algol, or even counterrotating triple systems like ζ Aqr (Tokovinin 2016b). Similarly, there exist non-coplanar exoplanetary systems such as ν And (McArthur et al 2010) and close binaries with misaligned stellar spins (Albrecht et al 2014). Dynamical interactions with other stars or planets are often evoked to explain the misalignment.…”

Section: Introductionmentioning

confidence: 99%

Relative Orbit Orientation in Several Resolved Multiple Systems

Tokovinin

Latham

2017

ApJ

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This work extends the still modest number of multiple stars with known relative orbit orientation. Accurate astrometry and radial velocities are used jointly to compute or update outer and inner orbits in three nearby triple systems HIP 101955 (orbital periods 38.68 and 2.51 years), HIP 103987 (19.20 and 1.035 years), HIP 111805 (30.13 and 1.50 years) and in one quadruple system HIP 2643 (periods 70.3, 4.85 and 0.276 years), all composed of solar-type stars. The masses are estimated from the absolute magnitudes and checked using the orbits. The ratios of outer to inner periods (from 14 to 20) and the eccentricities of the outer orbits are moderate. These systems are dynamically stable, but not very far from the stability limit. In three systems all orbits are approximately coplanar and have small eccentricity, while in HIP 101955 the inner orbit with e = 0.6 is highly inclined.

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NEW OBSERVATIONAL CONSTRAINTS ON THE υ ANDROMEDAE SYSTEM WITH DATA FROM THEHUBBLE SPACE TELESCOPEAND HOBBY-EBERLY TELESCOPE

Cited by 155 publications

References 82 publications

Secular Chaos and the Production of Hot Jupiters

Secular Chaos and the Production of Hot Jupiters

Trapping in three-planet resonances during gas-driven migration

Relative Orbit Orientation in Several Resolved Multiple Systems

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