The Solar system’s post-main-sequence escape boundary

Veras, Dimitri; Wyatt, M. C.

doi:10.1111/j.1365-2966.2012.20522.x

Cited by 80 publications

(66 citation statements)

References 58 publications

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“…During a star's main sequence lifetime, the star's mass and radius change negligibly. These changes translate into little dynamical excitation amongst orbiting bodies; Veras & Wyatt (2012) point out that the Solar system planets would increase their semimajor axes by at most about 0.055 per cent. Due to such small changes, the vast majority of all main sequence exoplanet studies treat the stellar mass and radius as fixed.…”

Section: Multi-planet Instabilitiesmentioning

confidence: 99%

Detectable close-in planets around white dwarfs through late unpacking

Veras

Gänsicke

2014

Monthly Notices of the Royal Astronomical Society

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119

129

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Although 25%-50% of white dwarfs (WDs) display evidence for remnant planetary systems, their orbital architectures and overall sizes remain unknown. Vibrant close-in (≃ 1R ⊙ ) circumstellar activity is detected at WDs spanning many Gyrs in age, suggestive of planets further away. Here we demonstrate how systems with 4 and 10 closely-packed planets that remain stable and ordered on the main sequence can become unpacked when the star evolves into a WD and experience pervasive inward planetary incursions throughout WD cooling. Our full-lifetime simulations run for the age of the Universe and adopt main sequence stellar masses of 1.5M ⊙ , 2.0M ⊙ and 2.5M ⊙ , which correspond to the mass range occupied by the progenitors of typical present-day WDs. These results provide (i) a natural way to generate an ever-changing dynamical architecture in post-main-sequence planetary systems, (ii) an avenue for planets to achieve temporary close-in orbits that are potentially detectable by transit photometry, and (iii) a dynamical explanation for how residual asteroids might pollute particularly old WDs.

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Section: Multi-planet Instabilitiesmentioning

confidence: 99%

Detectable close-in planets around white dwarfs through late unpacking

Veras

Gänsicke

2014

Monthly Notices of the Royal Astronomical Society

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119

129

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“…The resonant planetary systems emerging from the protoplanetary disks can become dynamically unstable after the gas disappears, leading to a phase where planets scatter each other. This model can help explain the observed resonant exoplanets (e.g., Gliese 876; Marcy et al 2001), commonly large exoplanet eccentricities (Weidenschilling & Marzari 1996;Rasio & Ford 1996), and microlensing data that show evidence for a large number of planets that are free-floating in interstellar space (Sumi et al 2011; but see Veras & Raymond 2012).…”

Section: Introductionmentioning

confidence: 98%

Statistical Study of the Early Solar System's Instability With Four, Five, and Six Giant Planets

Nesvorný

Morbidelli

2012

The Astronomical Journal

340

461

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Several properties of the solar system, including the wide radial spacing and orbital eccentricities of giant planets, can be explained if the early solar system evolved through a dynamical instability followed by migration of planets in the planetesimal disk. Here we report the results of a statistical study, in which we performed nearly 10 4 numerical simulations of planetary instability starting from hundreds of different initial conditions. We found that the dynamical evolution is typically too violent, if Jupiter and Saturn start in the 3:2 resonance, leading to ejection of at least one ice giant from the solar system. Planet ejection can be avoided if the mass of the transplanetary disk of planetesimals was large (M disk 50 M Earth ), but we found that a massive disk would lead to excessive dynamical damping (e.g., final e 55 0.01 compared to present e 55 = 0.044, where e 55 is the amplitude of the fifth eccentric mode in the Jupiter's orbit), and to smooth migration that violates constraints from the survival of the terrestrial planets. Better results were obtained when the solar system was assumed to have five giant planets initially, and one ice giant, with mass comparable to that of Uranus and Neptune, was ejected into interstellar space by Jupiter. The best results were obtained when the ejected planet was placed into the external 3:2 or 4:3 resonance with Saturn and M disk 20 M Earth . The range of possible outcomes is rather broad in this case, indicating that the present solar system is neither a typical nor expected result for a given initial state, and occurs, in best cases, with only a 5% probability (as defined by the success criteria described in the main text). The case with six giant planets shows interesting dynamics but does offer significant advantages relative to the five-planet case.

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“…This directly affects their planetary systems, in the most dramatic way since their formation. Their fate during the final stellar evolution stages has been the subject of several recent works (Veras 2016b;Staff et al 2016;Veras & Wyatt 2012;Schröder & Connon Smith 2008;Villaver & Livio 2007; see also the review by Veras 2016a). However, as AGB star planets are embedded in complex circumstellar envelopes and are vastly outshone by their parent star, the observation of this critical phase presents considerable and yet unsolved challenges.…”

Section: Introductionmentioning

confidence: 99%

ALMA observations of the nearby AGB star L₂ Puppis

Kervella

Homan

Richards

et al. 2016

A&A

133

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Six billion years from now, while evolving on the asymptotic giant branch (AGB), the Sun will metamorphose from a red giant into a beautiful planetary nebula. This spectacular evolution will impact the solar system planets, but observational confirmations of the predictions of evolution models are still elusive as no planet orbiting an AGB star has yet been discovered. The nearby AGB red giant L 2 Puppis (d = 64 pc) is surrounded by an almost edge-on circumstellar dust disk. We report new observations with ALMA at very high angular resolution (18 × 15 mas) in band 7 (ν ≈ 350 GHz) that allow us to resolve the velocity profile of the molecular disk. We establish that the gas velocity profile is Keplerian within the central cavity of the dust disk, allowing us to derive the mass of the central star L 2 Pup A, m A = 0.659 ± 0.011 ± 0.041 M (±6.6%). From evolutionary models, we determine that L 2 Pup A had a near-solar main-sequence mass, and is therefore a close analog of the future Sun in 5 to 6 Gyr. The continuum map reveals a secondary source (B) at a radius of 2 AU contributing f B / f A = 1.3 ± 0.1% of the flux of the AGB star. L 2 Pup B is also detected in CO emission lines at a radial velocity of v B = 12.2 ± 1.0 km s −1 . The close coincidence of the center of rotation of the gaseous disk with the position of the continuum emission from the AGB star allows us to constrain the mass of the companion to m B = 12 ± 16 M Jup . L 2 Pup B is most likely a planet or low-mass brown dwarf with an orbital period of about five years. Its continuum brightness and molecular emission suggest that it may be surrounded by an extended molecular atmosphere or an accretion disk. L 2 Pup therefore emerges as a promising vantage point on the distant future of our solar system.

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The Solar system’s post-main-sequence escape boundary

Cited by 80 publications

References 58 publications

Detectable close-in planets around white dwarfs through late unpacking

Detectable close-in planets around white dwarfs through late unpacking

Statistical Study of the Early Solar System's Instability With Four, Five, and Six Giant Planets

ALMA observations of the nearby AGB star L₂ Puppis

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The Solar system’s post-main-sequence escape boundary

Cited by 80 publications

References 58 publications

Detectable close-in planets around white dwarfs through late unpacking

Detectable close-in planets around white dwarfs through late unpacking

Statistical Study of the Early Solar System's Instability With Four, Five, and Six Giant Planets

ALMA observations of the nearby AGB star L2 Puppis

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Product

Resources

About

ALMA observations of the nearby AGB star L₂ Puppis