The secular evolution of the Kuiper belt after a close stellar encounter

Punzo, Davide; Capuzzo–Dolcetta, R.; Zwart, Simon Portegies

doi:10.1093/mnras/stu1650

Cited by 16 publications

(18 citation statements)

References 38 publications

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“…Simulations of the influence of a stellar flyby on a debris disc were also motivated to explain individual observed systems, for example in case of β Pictoris by Larwood & Kalas (2001) and HD 141569 by Reche et al (2009), or to understand the scattered Kuiper belt in the Solar system (e.g. Melita et al 2005;Kobayashi et al 2005;Punzo et al 2014). Results on the change of the disc mass or size due to the flybys were often applied in the simulations of star clusters, where the encounters occur (for example Olczak et al 2006;Pfalzner et al 2006;Lestrade et al 2011;Vincke et al 2015;Portegies Zwart 2016).…”

Section: Simulations Of Discs During Stellar Encountersmentioning

confidence: 99%

Mass transfer between debris discs during close stellar encounters

Jílková¹,

Hamers²,

Hammer³

et al. 2016

Mon. Not. R. Astron. Soc.

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We study mass transfers between debris discs during stellar encounters. We carried out numerical simulations of close flybys of two stars, one of which has a disc of planetesimals represented by test particles. We explored the parameter space of the encounters, varying the mass ratio of the two stars, their pericentre and eccentricity of the encounter, and its geometry. We find that particles are transferred to the other star from a restricted radial range in the disc and the limiting radii of this transfer region depend on the parameters of the encounter. We derive an approximate analytic description of the inner radius of the region. The efficiency of the mass transfer generally decreases with increasing encounter pericentre and increasing mass of the star initially possessing the disc. Depending on the parameters of the encounter, the transfer particles have a specific distributions in the space of orbital elements (semimajor axis, eccentricity, inclination, and argument of pericentre) around their new host star. The population of the transferred particles can be used to constrain the encounter through which it was delivered. We expect that many stars experienced transfer among their debris discs and planetary systems in their birth environment. This mechanism presents a formation channel for objects on wide orbits of arbitrary inclinations, typically having high eccentricity but possibly also close-to-circular (eccentricities of about 0.1). Depending on the geometry, such orbital elements can be distinct from those of the objects formed around the star.

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Section: Simulations Of Discs During Stellar Encountersmentioning

confidence: 99%

Mass transfer between debris discs during close stellar encounters

Jílková¹,

Hamers²,

Hammer³

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Among them are, for example, galaxy-galaxy encounters and perturbations of protoplanetary discs, debris discs, or planetary systems by passing stars (see e.g. Toomre & Toomre 1972;Farouki & Shapiro 1981;Clarke & Pringle 1993;Heller 1995;Hall et al 1996;Hall 1997;Kobayashi & Ida 2001;Melita et al 2002;Levison et al 2004;Pfalzner et al 2005b;Olczak et al 2006;Scharwächter et al 2007;Malmberg et al 2011;Craig & Krumholz 2013;Punzo et al 2014). Some of these processes happen on different scales and might involve additional forces, such as viscous friction or magnetic fields.…”

Section: Introductionmentioning

confidence: 99%

From star-disc encounters to numerical solutions for a subset of the restricted three-body problem

Breslau

Vincke

Pfalzner

2017

A&A

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Various astrophysical processes exist, where the fly-by of a massive object affects matter that is initially supported against gravity by rotation. Examples are perturbations of galaxies, protoplanetary discs, or planetary systems. We approximate such events as a subset of the restricted three-body problem by considering only perturbations of non-interacting low-mass objects that are initially on circular Keplerian orbits. In this paper, we present a new parametrisation of the initial conditions of this problem. Under certain conditions, the initial positions of the low-mass objects can be specified as being largely independent of the initial position of the perturber. In addition, exploiting the known scalings of the problem reduces the parameter space of initial conditions for one specific perturbation to two dimensions. To this two-dimensional initial condition space, we have related the final properties of the perturbed trajectories of the low-mass objects from our numerical simulations. In this way, maps showing the effect of the perturbation on the low-mass objects were created, which provide a new view on the perturbation process. Comparing the maps for different mass-ratios reveals that the perturbations by low-and high-mass perturbers are dominated by different physical processes. The equal-mass case is a complicated mixture of the other two cases. Since the final properties of trajectories with similar initial conditions are also usually similar, the results of the limited number of integrated trajectories can be generalised to the full presented parameter space by interpolation. Since our results are also unique within the accuracy strived for, they constitute general numerical solutions for this subset of the restricted three-body problem. As such, they can be used to predict the evolution of real physical problems by simple transformations, such as scaling, without further simulations. Possible applications are the perturbation of protoplanetary discs or planetary systems by the fly-by of another star. Here, the maps enable us, for example, to quantify the portion of unbound material for any periastron distance without the need for further simulations.

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“…According to this model the violent and rather sudden migration of Uranus and Neptune would have excited the cold Kuiper belt (Brasser et al 2012). This reorganization of the outer giant planets would have initiated the hot Kuiper belt (Levison et al 2008) that, due to the long local relaxation time, cools down only very slowly (Punzo et al 2014). Subsequent chaotic diffusion (Morbidelli et al 2008), perturbations in the Sun's birth environment in close flybys (Davies et al 2014), or more distant encounters could have caused further migration of the Kuiper-belt objects to orbits similar to that of Sedna (Brasser et al 2012).…”

Section: Introductionmentioning

confidence: 99%

How Sedna and family were captured in a close encounter with a solar sibling

Jílková

Zwart

Pijloo

et al. 2015

Mon. Not. R. Astron. Soc.

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The discovery of 2012 VP 113 initiated the debate on the origin of the Sedna family of planetesimals in orbit around the Sun. Sednitos roam the outer regions of the Solar system between the Egeworth-Kuiper belt and the Oort cloud, in extraordinary wide (a > 150 au) orbits with a large perihelion distance of q > 30 au compared to the Earth's (a ≡ 1 au and eccentricity e ≡ (1 − q/a) 0.0167 or q 1 au). This population is composed of a dozen objects, which we consider a family because they have similar perihelion distance and inclination with respect to the ecliptic i = 10 • -30 • . They also have similar argument of perihelion ω = 340 • ± 55 • . There is no ready explanation for their origin. Here we show that these orbital parameters are typical for a captured population from the planetesimal disk of another star. Assuming the orbital elements of Sednitos have not changed since they acquired their orbits, we reconstruct the encounter that led to their capture. We conclude that they might have been captured in a near miss with a 1.8 M star that impacted the Sun at 340 au at an inclination with respect to the ecliptic of 17-34 • with a relative velocity at infinity of ∼ 4.3 km/s. We predict that the Sednitos-region is populated by 930 planetesimals and the inner Oort cloud acquired ∼ 440 planetesimals through the same encounter.

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The secular evolution of the Kuiper belt after a close stellar encounter

Cited by 16 publications

References 38 publications

Mass transfer between debris discs during close stellar encounters

Mass transfer between debris discs during close stellar encounters

From star-disc encounters to numerical solutions for a subset of the restricted three-body problem

How Sedna and family were captured in a close encounter with a solar sibling

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