Relative velocities among accreting planetesimals in binary systems: The circumprimary case

Thébault, P.; Marzari, F.; Scholl, H.

doi:10.1016/j.icarus.2006.01.022

Cited by 158 publications

(309 citation statements)

References 30 publications

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“…In reality, however, only a small fraction of water would be accreted onto a planet (or planetary system) inside the HZ. Indeed, both the real position of the planet on its orbit and the impact velocity of these HZc are crucial parameters in collisional material transport as pointed out by Thébault et al (2006) and Leinhardt & Stewart (2012). A fully self-consistent modelling of the water delivery at impact lies beyond the scope of the current work, however.…”

Section: The Water Mass Fraction Of Incoming Hzcmentioning

confidence: 94%

“…The question whether habitable worlds can actually exist in such environments is, therefore, not a trivial one. Previous works on early stages of planetary formation show that planetesimal accretion can be more difficult than in single star systems (Thebault & Haghighipour 2014, and references therein). This in turn can question the possibility of whether embryos form in such systems.…”

Section: Introductionmentioning

confidence: 99%

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Asteroid flux towards circumprimary habitable zones in binary star systems

Bancelin

Pilat-Lohinger

Eggl

et al. 2015

A&A

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Context. So far, more than 130 extrasolar planets have been found in multiple stellar systems. Dynamical simulations show that the outcome of the planetary formation process can lead to different planetary architecture (i.e. location, size, mass, and water content) when the star system is single or double. Aims. In the late phase of planetary formation, when embryo-sized objects dominate the inner region of the system, asteroids are also present and can provide additional material for objects inside the habitable zone (HZ). In this study, we make a comparison of several binary star systems and how efficient they are at moving icy asteroids from beyond the snow line into orbits crossing the HZ. Methods. We modelled a belt of 10 000 asteroids (remnants from the late phase of the planetary formation process) beyond the snow line. The planetesimals are placed randomly around the primary star and move under the gravitational influence of the two stars and a gas giant. As the planetesimals do not interact with each other, we divided the belt into 100 subrings which were integrated separately. In this statistical study, several double star configurations with a G-type star as primary are investigated. Results. Our results show that small bodies also participate in bearing a non-negligible amount of water to the HZ. The proximity of a companion moving on an eccentric orbit increases the flux of asteroids to the HZ, which could result in a more efficient water transport on a short timescale, causing a heavy bombardment. In contrast to asteroids moving under the gravitational perturbations of one G-type star and a gas giant, we show that the presence of a companion star not only favours a faster depletion of our disk of planetesimals, but can also bring 4-5 times more water into the whole HZ.

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Section: The Water Mass Fraction Of Incoming Hzcmentioning

confidence: 94%

Section: Introductionmentioning

confidence: 99%

Asteroid flux towards circumprimary habitable zones in binary star systems

Bancelin

Pilat-Lohinger

Eggl

et al. 2015

A&A

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“…However, some questions are still actively debated, A&A 524, A13 (2010) in particular regarding the earlier stage leading from kilometresized planetesimals to the embryos (e.g. Thébault et al 2006Thébault et al , 2009Paardekooper et al 2008;Xie & Zhou 2009;Paardekooper & Leinhardt 2010).…”

Section: Planets and Discs In Binariesmentioning

confidence: 99%

Debris discs in binaries: a numerical study

Thébault

Marzari

Augereau

2010

A&A

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Context. Debris disc analysis and modelling provide crucial information about the structure and the processes at play in extrasolar planetary systems. In binary systems, this issue is more complex because the disc should also respond to the companion star's perturbations. Aims. We explore the dynamical evolution of a collisionally active debris disc for different initial parent body populations, diverse binary configurations, and optical depths. We focus on the radial extent and size distribution of the disc in a stationary state. Methods. We numerically followed the evolution of 10 5 massless small grains, initially produced from a circumprimary disc of parent bodies following a size distribution in dN ∝ s −3.5 ds . Grains were submitted to both stars' gravity and radiation pressure. In addition, particles were assigned an empirically derived collisional lifetime. Results. For all the binary configurations, the disc extends far beyond the critical semi-major axis a crit for orbital stability. This is due to the steady production of small grains, placed by radiation pressure on eccentric orbits reaching beyond a crit . The amount of matter beyond a crit depends on the balance between collisional production and dynamical removal rates: it increases for more massive discs, as well as for eccentric binaries. Another important effect is that, in the dynamically stable region, the disc is depleted from its smallest grains. Both results could lead to observable signatures. Conclusions. We have shown that a companion star can never fully truncate a collisionally active disc. For eccentric companions, grains in the unstable regions can contribute significantly to the thermal emission in the mid-IR. Discs with sharp outer edges, especially bright ones such as HR4796A, are probably shaped by other mechanisms.

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confidence: 99%

Possible planet formation in the young, low-mass, multiple stellar system GG Tau A

Dutrey

Folco

Guilloteau

et al. 2014

Nature

105

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Forming planets around binary stars may be more difficult than around single stars [1][2][3] . In a close binary star (< 100 au separation), theory predicts the presence of circumstellar discs around each star, and an outer circumbinary disc surrounding a gravitationally cleared inner cavity 4,5 . As the inner discs are depleted by accretion onto the stars on timescales of few 10 3 yr, replenishing material must be transferred from the outer reservoir in order to fuel 1 planet formation (which occurs on timescales of ∼1 Myr). Gas flowing through disc cavities has been detected in single star systems 6 . A circumbinary disc was discovered around the young low-mass binary system GGTau-A 7 , which has recently been proven to be a hierarchical triple system 8 . It has one large inner disc 9 around the southern single star and shows small amounts of shocked H 2 gas residing within the central cavity 10 , but other than a weak detection 11 , hitherto the distribution of cold gas in this cavity or in any other binary or multiple star system has never been determined. Here we report imaging of massive CO-emitting gas fragments within the GG Tau-A cavity. From the kinematics we conclude that the flow appears capable of sustaining the inner disc beyond the accretion lifetime, leaving time for planet formation to occur.The 1-5 Million year old 12, 13 triple stellar system GGTau-A is located at 140 pc in a hole of the Taurus molecular cloud. Its molecular emission is free of contamination 14 and there is no known outflow neither jet associated to the source. The main binary GGTau-A (Aa-Ab) and the close-binary GGTau-Ab (Ab1-Ab2) have an apparent separation of 35 au and 4.5 au, respectively 8 .The outer circumbinary Keplerian disc of gas and dust surrounding GGTau-A consists of a ring extending from radius r ∼ 190 to 280 au and an outer disc extending up to 800 au from the central stars with a total mass ∼ 0.15 M ⊙ 14 .Using the Atacama Large Millimetre Array (ALMA), we observed GGTau-A in the dust thermal emission at 0.45 mm and in CO J=6-5 line ( Fig.1: panels a,b,c) with an angular resolution θ ≃ 0.25 ′′ or ∼35 au. The continuum image shows cold dust emission from only one circumstellar 2 disc-like structure associated with GGTau-Aa 9, 15 . We estimate the minimum dust disc size to be ∼ 7 au while the minimum mass of gas and dust is roughly 10 −3 M ⊙ about Jupiter's mass. The complex CO J=6-5 spectral line shape at the location of GGTau-Aa also reveals the existence of a CO circumstellar disc of outer radius ∼ 20 au (Methods and Extended Data: Fig.2). We do not detect cold dust emission around GGTau-Ab even though the existence of inner dust disc(s) was reported from unresolved Infrared emission 16 . Our 0.45 mm upper limits (Methods) are compatible with tidal truncation which prevents any circumstellar disc to extend beyond about 2 au 8 .The ALMA CO J=6-5 image ( Fig.1 panels a,b,c and Extended Data: Fig.1 and Fig.2) also clearly resolves CO gas within the central cavity with a structure indicative of the streamer-like f...

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Relative velocities among accreting planetesimals in binary systems: The circumprimary case

Cited by 158 publications

References 30 publications

Asteroid flux towards circumprimary habitable zones in binary star systems

Asteroid flux towards circumprimary habitable zones in binary star systems

Debris discs in binaries: a numerical study

Possible planet formation in the young, low-mass, multiple stellar system GG Tau A

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