QYMSYM: A GPU-accelerated hybrid symplectic integrator that permits close encounters

Moore, Alexander; Quillen, Alice C.

doi:10.1016/j.newast.2011.03.009

Cited by 21 publications

(23 citation statements)

References 15 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For these problems symplectic integrators based on Hamiltonian splitting (Wisdom and Holman, 1991) are used, using the fact that the dynamics is dominated by a central object. For close encounters between objects orbiting the central body, additional splitting methods have been developed involving the interaction terms between orbiters (Chambers, 1999;Duncan et al, 1998;Moore and Quillen, 2011).…”

Section: Introductionmentioning

confidence: 99%

N-body integrators with individual time steps from Hierarchical splitting

2012

View full text Add to dashboard Cite

We review the implementation of individual particle time-stepping for N-body dynamics. We present a class of integrators derived from second order Hamiltonian splitting. In contrast to the usual implementation of individual time-stepping, these integrators are momentum conserving and show excellent energy conservation in conjunction with a symmetrized time step criterion. We use an explicit but approximate formula for the time symmetrization that is compatible with the use of individual time steps. No iterative scheme is necessary. We implement these ideas in the HUAYNO 1 code and present tests of the integrators and show that the presented integration schemes shows good energy conservation, with little or no systematic drift, while conserving momentum and angular momentum to machine precision for long term integrations.

show abstract

Section: Introductionmentioning

confidence: 99%

N-body integrators with individual time steps from Hierarchical splitting

2012

View full text Add to dashboard Cite

show abstract

“…Final positions of the planets a 1, f and a 2, f and the total number of orbit‐crossing planetesimals, N c , are also listed in Table . The change in total energy due to numerical integration errors at the end of the integrations was |Δ E / E 0 | ≲ 10 −4 , where E 0 is the initial energy (see Moore & Quillen for a discussion about the accuracy of this integrator). The simulations were run using nvidia graphics cards from the GT200 architecture (the Quadro FX 5800 or the GTX 285) or using Fermi Class Tesla C2050 cards from the GF100 architecture.…”

Section: Close Encounter Distribution For a Migrating Two‐planet Systemmentioning

confidence: 99%

“…We have modified the hybrid symplectic integrator qymsym (Moore & Quillen ) to record properties of all particles that approach within a Hill radius of a planet. The integrator runs at two levels.…”

Section: Close Encounter Distribution For a Migrating Two‐planet Systemmentioning

confidence: 99%

Capture of irregular satellites via binary planetesimal exchange reactions in migrating planetary systems

Quillen

Hasan

Moore

2012

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

By logging encounters between planetesimals and planets, we compute the distribution of encounters in a numerically integrated two‐planet system that is migrating due to interactions with an exterior planetesimal belt. Capture of an irregular satellite in orbit about a planet through an exchange reaction with a binary planetesimal is only likely when the binary planetesimal undergoes a slow and close encounter with the planet. Taking care to consider where a planet‐orbit‐crossing binary planetesimal would first be tidally disrupted, we estimate the probability of both tidal disruption and irregular satellite capture. We estimate that the probability that the secondary of a binary planetesimal is captured and becomes an irregular satellite about a Neptune mass outer planet is about 1/100 for binaries with masses and separations similar to transneptunian planetesimal binaries. Scaling functions are given allowing probabilities to be estimated for satellite capture from binary planetesimals with other masses, mass ratios and separations. This capture probability is only weakly dependent upon the binary's tidal disruption radius. We find that the probability that a satellite is captured by the inner planet is one to two orders of magnitude lower than by the outer planet. If young exoplanetary debris discs contain a population of binary planetesimals, then an outwards migrating outer planet should host a recently captured irregular satellite population.

show abstract

“…Fan & Batygin (2017) investigated the effect of planetesimal self-gravity on the evolution of giant planets' and Kuiper Belt objects' orbits. They used QYM-SYM GPU-based N-body code (Moore & Quillen 2011) and compared self-interacting to non-self-interacting models, which contain 1000 planetesimals and the four giant planets. The orbital architecture of the final systems was similar, however, instabilities led to the destruction of the system in more cases with self-interacting models than with non-self-interacting ones.…”

Section: Introductionmentioning

confidence: 99%

Oligarchic growth in a fully interacting system

Dencs

Regály

2021

A&A

View full text Add to dashboard Cite

Context. In the oligarchic growth model, protoplanets develop in the final stage of planet formation via collisions between planetesimals and planetary embryos. The majority of planetesimals are accreted by the embryos, while the remnant planetesimals acquire dynamically excited orbits. The efficiency of planet formation can be defined by the mass ratio between formed protoplanets and the initial mass of the embryo-planetesimal belt. Aims. In numerical simulations of the oligarchic growth, the gravitational interactions between planetesimals are usually neglected due to computational difficulties. In this way, computations require fewer resources. We investigated the effect of this simplification by modeling the planet formation efficiency in a belt of embryos with self-interacting or non-self-interacting planetesimals. Methods. We used our own graphics processing unit-based direct N-body integrator for the simulations. We compared 2D models using different initial embryo numbers, different initial planetesimal numbers, and different total initial belt masses. For a limited number of cases, we compared the 2D and 3D simulations. Results. We found that planet formation efficiency is higher if the planetesimal self-interaction is taken into account in models that contain the commonly used 100 embryos. The observed effect can be explained by the damping of planetesimal eccentricities by their self-gravity. The final numbers of protoplanets are independent of planetesimal self-gravity, while the average mass of the formed protoplanets is larger in the self-interacting models. We also found that the non-self-interacting and self-interacting models qualitatively give the same results above 200 embryos. Our findings show that the higher the initial mass of the embryo-planetesimal belt, the higher the discrepancy between models that use self-interacting or non-self-interacting planetesimals is. The study of 3D models showed quantitatively the same results as the 2D models for low average inclination. We conclude that it is important to include planetesimal self-interaction in both 2D and 3D models in cases where the initial embryo number is less than 200.

show abstract

QYMSYM: A GPU-accelerated hybrid symplectic integrator that permits close encounters

Cited by 21 publications

References 15 publications

N-body integrators with individual time steps from Hierarchical splitting

N-body integrators with individual time steps from Hierarchical splitting

Capture of irregular satellites via binary planetesimal exchange reactions in migrating planetary systems

Oligarchic growth in a fully interacting system

Contact Info

Product

Resources

About