Multiplanet destabilization and escape in post-main-sequence systems

Voyatzis, George; Hadjidemetriou, John D.; Veras, Dimitri; Varvoglis, H.

doi:10.1093/mnras/stt137

Cited by 94 publications

(78 citation statements)

References 68 publications

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“…We consider the possible implications of the stellar mass loss for planetary dynamics and show that, for small values, the stability of the planetary motion is not affected. This result is in agreement with the results obtained by Voyatzis et al (2013), which showed that the planetary motion is destabilized when the loss of the stellar mass reaches 10%.…”

Section: Introductionsupporting

confidence: 93%

Formation and evolution of the two 4/3 resonant giants planets in HD 200964

Santos

Correa-Otto

Michtchenko

et al. 2014

A&A

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Context. It has been suggested that HD 200964 is the first exoplanetary system with two Jovian planets evolving in the 4/3 meanmotion resonance (MMR). Previous scenarios to simulate the formation of two giant planets in the stable 4/3 resonance configuration have failed. Moreover, the orbital parameters available in the literature point out an unstable configuration of the planetary pair. Aims. The purpose of this paper is i) to determine the orbits of the planets from the radial velocity measurements and update the value of the stellar mass (1.57 M ); ii) to analyse the stability of the planetary evolution in the vicinity and inside the 4/3 MMR; and iii) to elaborate a possible scenario for the formation of systems in the 4/3 MMR. Methods. We use a previous model to simulate the formation of the stable planetary pair trapped inside the 4/3 resonance. Our scenario includes an interaction between the type I and type II of migration, planetary growth and stellar evolution from the main sequence to the sub-giant branch. The redetermination of the orbits is done using a biased Monte Carlo procedure, while the planetary dynamics is studied using numerical tools, such as dynamical maps and dynamical power spectra. Results. The results of the formation simulations are able to very closely reproduce the 4/3 resonant dynamics of the best-fit configuration obtained in this paper. Moreover, the confidence interval of the fit matches well with the very narrow stable region of the 4/3 MMR. Conclusions. The formation process of the HD 200964 system is very sensitive to the planetary masses and protoplanetary disk parameters. Only a thin, flat disk allows the embryo-sized planets to reach the 4/3 resonant configuration. The stable evolution of the resonant planets is also sensitive to the mass of the central star, because of overlapping high-order resonances inside the 4/3 resonance. Regardless of the very narrow domain of stable motion, the confidence interval of our fit closely matches the stability area.

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Section: Introductionsupporting

confidence: 93%

Formation and evolution of the two 4/3 resonant giants planets in HD 200964

Santos

Correa-Otto

Michtchenko

et al. 2014

A&A

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“…For instance, gravitational interactions between the planets can play an important role during the subgiant phase, although they tend to destabilize the system (Voyatzis et al 2013;Veras et al 2013;Mustill et al 2014). However, mean motion resonances (MMR) can help the inner orbit to migrate outward and thus escape being engulfed by the star, as in the formation of the solar system (e.g., Levison & Morbidelli 2003;D'Angelo & Marzari 2012).…”

Section: Discussionmentioning

confidence: 99%

Close-in planets around giant stars

Lillo-Box

Barrado

Correia

2016

A&A

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Extrasolar planets abound in almost any possible configuration. However, until five years ago, there was a lack of planets orbiting closer than 0.5 au to giant or subgiant stars. Since then, recent detections have started to populated this regime by confirming 13 planetary systems. We discuss the properties of these systems in terms of their formation and evolution off the main sequence. Interestingly, we find that 70.0 ± 6.6% of the planets in this regime are inner components of multiplanetary systems. This value is 4.2σ higher than for main-sequence hosts, which we find to be 42.4 ± 0.1%. The properties of the known planets seem to indicate that the closest-in planets (a < 0.06 au) to main-sequence stars are massive (i.e., hot Jupiters) and isolated and that they are subsequently engulfed by their host as it evolves to the red giant branch, leaving only the predominant population of multiplanetary systems in orbits 0.06 < a < 0.5 au. We discuss the implications of this emerging observational trend in the context of formation and evolution of hot Jupiters.

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“…Initially focusing on the future of the solar system (Sackmann et al 1993;Duncan & Lissauer 1998), a number of theoretical studies have shown that a fraction of planets can survive the red-giant stage Table 1 is available in electronic form at http://www.aanda.org of their host stars (Villaver & Livio 2007, 2009Nordhaus et al 2010;Mustill & Villaver 2012). The ensuing long-term orbital evolution is complex and may lead to planet ejections or collisions (Debes & Sigurdsson 2002;Veras et al 2011;Voyatzis et al 2013). Smaller bodies are likely to be scattered, from locations comparable to the solar system's main asteroid belt or Kuiper belt Debes et al 2012), which will lead to their tidal disruption if their trajectory takes them within the Roche radius of the white dwarf, ≈1 R , (Davidsson 1999).…”

Section: Introductionmentioning

confidence: 99%

The frequency of planetary debris around young white dwarfs

Koester

Gänsicke

Farihi

2014

A&A

442

531

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Context. Heavy metals in the atmospheres of white dwarfs are thought in many cases to be accreted from a circumstellar debris disk, which was formed by the tidal disruption of a rocky planetary body within the Roche radius of the star. The abundance analysis of photospheric elements and conclusions about the chemical composition of the accreted matter are a new and promising method of studying the composition of extrasolar planetary systems. However, ground-based searches for metal-polluted white dwarfs that rely primarily on the detection of the Ca ii K line become insensitive at T eff > 15 000 K because this ionization state depopulates.Aims. We present the results of the first unbiased survey for metal pollution among hydrogen-atmosphere (DA type) white dwarfs with cooling ages in the range 20-200 Myr and 17 000 K < T eff < 27 000 K. Methods. The sample was observed with the Cosmic Origins Spectrograph on board the Hubble Space Telescope in the far ultraviolet range between 1130 and 1435 Å. The atmospheric parameters were obtained using these spectra and optical observations from the literature. Element abundances were determined using theoretical models, which include the effects of element stratification due to gravitational settling and radiative levitation. Results. We find 48 of the 85 DA white dwarfs studied, or 56% show traces of heavy elements. In 25 stars (showing only Si and occasionally C), the elements can be explained by radiative levitation alone, although we argue that accretion has very likely occurred recently. The remaining 23 white dwarfs (27%), however, must be currently accreting. Together with previous studies from the ground and adopting bulk Earth abundances for the debris, accretion rates range from a few 10 5 g s −1 to a few 10 8 g s −1 , with no evident trend in cooling age from ≈40 Myr to ≈2 Gyr. Only a single, modest case of metal pollution (Ṁ < 10 6 g s −1 ) is found among ten white dwarfs with T eff > 23 000 K, in excellent agreement with the absence of infrared excess from dust around these warmer stars. The median, main sequence progenitor of our sample corresponds to an A-type star of ≈2 M , and we find 13 of 23 white dwarfs descending from main sequence 2-3 M , late B-and A-type stars to be currently accreting. Only one of 14 targets with M wd > 0.8 M is found to be currently accreting, which suggests a large fraction of these stars result from double-degenerate mergers, and the merger disks do not commonly reform large planetesimals or otherwise pollute the remnant. We reconfirm our previous finding that two 625 Myr Hyades white dwarfs are currently accreting rocky planetary debris. Conclusions. At least 27% of all white dwarfs with cooling ages 20-200 Myr are accreting planetary debris, but that fraction could be as high as ≈50%. At T eff > 23 000 K, the luminosity of white dwarfs is probably sufficient to vaporize circumstellar dust grains, so no stars with strong metal-pollution are found. Planetesimal disruption events should occur in this cooling age and temper...

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Multiplanet destabilization and escape in post-main-sequence systems

Cited by 94 publications

References 68 publications

Formation and evolution of the two 4/3 resonant giants planets in HD 200964

Formation and evolution of the two 4/3 resonant giants planets in HD 200964

Close-in planets around giant stars

The frequency of planetary debris around young white dwarfs

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