On the tidal evolution of Hot Jupiters on inclined orbits

Barker, Adrian J.; Ogilvie, Gordon I.

doi:10.1111/j.1365-2966.2009.14694.x

Cited by 228 publications

(317 citation statements)

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“…Since younger stars are known to rotate more rapidly than those matured, gravity darkening is available to unveil the distribution of φ for the younger systems by the future observations. Although tidal evolution of φ causes the initial memory on the formation process of hot Jupiters to be lost (Barker & Ogilvie 2009, Lai 2012, Xue et al 2014, one can minimize this undesirable effect by preferentially selecting younger systems as targets to measure φ. These aspects suggest that gravity-darkening (combined with nodal precession, if possible) model is very useful to study the formation scenario of close-in planets.…”

Section: Summary and Discussionmentioning

confidence: 99%

“…Tidal evolution of the system is computed by numerical integration of equations (19) - (21) in Correia et al (2011). The efficiency of tidal effect is also represented by the reduced tidal quality factor Q, which is written in terms of the above parameters as Q ≡ 3 4nk2∆t (Barker & Ogilvie 2009, Lai 2012, Rogers & Lin 2013, Xue et al 2014. We adopt our short solution as initial conditions and the values of Love number and tidal delay time estimated for Sun-like stars (k 2 = 0.028 and ∆t = 0.1 s following Correia et al 2011, which gives Q ∼ 10 6 for an orbital period of 0.448413 days).…”

Section: Long-term Dynamical Stabilitymentioning

confidence: 99%

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Revisiting a gravity-darkened and precessing planetary system PTFO 8-8695: A spin–orbit non-synchronous case

Kamiaka

Masuda

Xue

et al. 2015

Publications of the Astronomical Society of Japan

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We reanalyse the time-variable lightcurves of the transiting planetary system PTFO 8-8695, in which a planet of 3 to 4 Jupiter mass orbits around a rapidly rotating pre-main-sequence star. Both the planetary orbital period P orb of 0.448 days and the stellar spin period P s less than 0.671 days are unusually short, which makes PTFO 8-8695 an ideal system to check the model of gravity darkening and nodal precession. While the previous analysis of PTFO 8-8695 assumed that the stellar spin and planetary orbital periods are the same, we extend the analysis by discarding the spin-orbit synchronous condition, and find three different classes of solutions roughly corresponding to the nodal precession periods of 199±16, 475±21, and 827 ± 53 days that reproduce the transit lightcurves observed in 2009 and 2010. We compare the predicted lightcurves of the three solutions against the photometry data of a few percent accuracy obtained at Koyama Astronomical Observatory in 2014 and 2015, and find that the solution with the precession period of 199 ± 16 days is preferred even though preliminary. Future prospect and implications to other transiting systems are briefly discussed.

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Section: Summary and Discussionmentioning

confidence: 99%

Section: Long-term Dynamical Stabilitymentioning

confidence: 99%

Revisiting a gravity-darkened and precessing planetary system PTFO 8-8695: A spin–orbit non-synchronous case

Kamiaka

Masuda

Xue

et al. 2015

Publications of the Astronomical Society of Japan

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“…where Q is the equivalent tidal dissipation factor in the star (defined as 3/2Q /k 2, * , where Q is the standard tidal dissipation factor and k 2,1 its Love number -see Barker & Ogilvie 2009). Using the parameters from Table 2 we obtain:…”

Section: Tidal Evolutionmentioning

confidence: 99%

“…Specifically, the inward migration timescale for a planet of mass M p in a circular orbit of period P around a star of mass M , radius R and spin period P is (Barker & Ogilvie 2009):…”

Section: Tidal Evolutionmentioning

confidence: 99%

The secondary eclipses of WASP-19b as seen by the ASTEP 400 telescope from Antarctica

Abe

Gonçalves

Agabi

et al. 2013

A&A

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Aims. The Antarctica Search for Transiting ExoPlanets (ASTEP) program was originally aimed at probing the quality of the Dome C, Antarctica for the discovery and characterization of exoplanets by photometry. In the first year of operation of the 40 cm ASTEP 400 telescope (austral winter 2010), we targeted the known transiting planet WASP-19b in order to try to detect its secondary transits in the visible. This is made possible by the excellent sub-millimagnitude precision of the binned data. Methods. The WASP-19 system was observed during 24 nights in May 2010. Once brought back from Antarctica, the data were processed using various methods, and the best results were with an implementation of the optimal image subtraction (OIS) algorithm. Results. The photometric variability level due to starspots is about 1.8% (peak-to-peak), in line with the SuperWASP data from 2007 (1.4%) and higher than in 2008 (0.07%). We find a rotation period of WASP-19 of 10.7 ± 0.5 days, in agreement with the SuperWASP determination of 10.5 ± 0.2 days. Theoretical models show that this can only be explained if tidal dissipation in the star is weak, i.e. the tidal dissipation factor Q > 3 × 10 7 . Separately, we find evidence of a secondary eclipse of depth 390 ± 190 ppm with a 2.0σ significance, a phase that is consistent with a circular orbit and a 3% false positive probability. Given the wavelength range of the observations (420 to 950 nm), the secondary transit depth translates into a day-side brightness temperature of 2690 +150 −220 K, in line with measurements in the z and K bands. The day-side emission observed in the visible could be due either to thermal emission of an extremely hot day side with very little redistribution of heat to the night side or to direct reflection of stellar light with a maximum geometrical albedo A g = 0.27 ± 0.13. We also report a low-frequency oscillation in phase at the planet orbital period, but with a lower limit amplitude that could not be attributed to the planet phase alone and that was possibly contaminated with residual lightcurve trends.Conclusions. This first evidence of a secondary eclipse in the visible from the ground demonstrates the high potential of Dome C, Antarctica, for continuous photometric observations of stars with exoplanets. These continuous observations are required to understand star-planet interactions and the dynamical properties of exoplanetary atmospheres.

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“…The effect of the coupling between tides and magnetic braking on the evolution of short-period extrasolar planetary systems was studied by Barker & Ogilvie 2009. They found that neglecting magnetic braking in this type of systems results in a very different outcome of the evolution.…”

Section: Introductionmentioning

confidence: 99%

The coupled effect of tides and stellar winds on the evolution of compact binaries

Repetto

Nelemans

2014

Monthly Notices of the Royal Astronomical Society

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We follow the evolution of compact binaries under the coupled effect of tides and stellar winds until the onset of Roche-lobe overflow. These binaries contain a compact object (either a black-hole, a neutron-star, or a planet) and a stellar component. We integrate the full set of tidal equations, which are based on Hut's model for tidal evolution, and we couple them with the angular momentum loss in a stellar wind. Our aim is twofold. Firstly, we wish to highlight some interesting evolutionary outcomes of the coupling. When tides are coupled with a non-massive stellar wind, one interesting outcome is that in certain types of binaries, the stellar spin tends to reach a quasi-equilibrium state, where the effect of tides and wind are counteracting each other. When tides are coupled with a massive wind, we parametrize the evolution in terms of the decoupling radius, at which the wind decouples from the star. Even for small decoupling radii this wind braking can drive systems on the main sequence to Roche-lobe overflow that otherwise would fail to do so. Our second aim is to inspect whether simple timescale considerations are a good description of the evolution of the systems. We find that simple timescale considerations, which rely on neglecting the coupling between tides and stellar winds, do not accurately represent the true evolution of compact binaries. The outcome of the coupled evolution of the rotational and orbital elements can strongly differ from simple timescale considerations, as already pointed out by Barker & Ogilvie 2009 in the case of short-period planetary systems.

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On the tidal evolution of Hot Jupiters on inclined orbits

Cited by 228 publications

References 54 publications

Revisiting a gravity-darkened and precessing planetary system PTFO 8-8695: A spin–orbit non-synchronous case

Revisiting a gravity-darkened and precessing planetary system PTFO 8-8695: A spin–orbit non-synchronous case

The secondary eclipses of WASP-19b as seen by the ASTEP 400 telescope from Antarctica

The coupled effect of tides and stellar winds on the evolution of compact binaries

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