The Astrophysical Multipurpose Software Environment

Pelupessy, F. I.; Elteren, A. van; Vries, Nathan de; McMillan, Stephen L. W.; Drost, Niels; Zwart, Simon Portegies

doi:10.1051/0004-6361/201321252

Cited by 209 publications

(225 citation statements)

References 68 publications

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“…Here, we used the updated code SecularMultiple (Hamers & Portegies Zwart 2016) interfaced in the AMUSE framework (Portegies Zwart et al 2013;Pelupessy et al 2013). The SecularMultiple code applies to arbitrary hierarchies and numbers of bodies; evidently, its underlying algorithm reduces to the same equations for four bodies.…”

Section: Secular Dynamicsmentioning

confidence: 99%

On the formation of hot and warm Jupiters via secular high-eccentricity migration in stellar triples

Hamers

2017

Mon. Not. R. Astron. Soc.

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Hot Jupiters (HJs) are Jupiter-like planets orbiting their host star in tight orbits of a few days. They are commonly believed not to have formed in situ, requiring inwards migration towards the host star. One of the proposed migration scenarios is secular high-eccentricity or high-e migration, in which the orbit of the planet is perturbed to high eccentricity by secular processes, triggering strong tidal evolution and orbital migration. Previous theoretical studies have considered secular excitation in stellar binaries. Recently, a number of HJs have been observed in stellar triple systems. In the latter, the secular dynamics are much richer compared to stellar binaries, and HJs could potentially be formed more efficiently. Here, we investigate this possibility by modeling the secular dynamical and tidal evolution of planets in two hierarchical configurations in stellar triple systems. We find that the HJ formation efficiency is higher compared to stellar binaries, but only by at most a few tens of per cent. The orbital properties of the HJs formed in the simulations are very similar to HJs formed in stellar binaries, and similarly to studies of the latter we find no significant number of warm Jupiters. HJs are only formed in our simulations for triples with specific orbital configurations, and our constraints are approximately consistent with current observations. In future, this allows to rule out high-e migration in stellar triples if a HJ is detected in a triple grossly violating these constraints.

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Section: Secular Dynamicsmentioning

confidence: 99%

On the formation of hot and warm Jupiters via secular high-eccentricity migration in stellar triples

Hamers

2017

Mon. Not. R. Astron. Soc.

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“…In order to couple the gravitational N-body code to the gas particles we use the AMUSE bridge. The bridge module provides a selfconsistent coupling between different components of a selfgravitating system using operator splitting (see Fujii et al 2007;Pelupessy & Portegies Zwart 2012;Pelupessy et al 2013). In short, with bridge the gas and stars are integrated in each other's mutual gravitational field.…”

Section: Gravitational Integrationmentioning

confidence: 99%

Stellar winds near massive black holes – the case of the S-stars

Lützgendorf

Helm

Pelupessy

et al. 2016

Mon. Not. R. Astron. Soc.

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The Galactic center provides a unique laboratory to study the interaction of a supermassive black hole (SMBH) with its gaseous and stellar environment. Simulations to determine the accretion of stellar winds from the surrounding O-stars onto the black hole have been performed earlier, but in those the presence of the S-star system was ignored. The S-stars are a group of young massive B-stars in relatively close orbits around the black hole. Here we simulate those stars in order to study their contribution to the accretion rate, without taking the more distant and massive O-stars into account. We use the Astrophysical Multi-purpose Software Environment (AMUSE) to combine gravitational physics, stellar evolution and hydrodynamics in a single simulation of the S-stars orbiting the supermassive black hole, and use this framework to determine the amount of gas that is accreted onto the black hole. We find that the accretion rate is sensitive to the wind properties of the S-stars (rate of mass-loss and terminal velocity). Our simulations are consistent with the observed accretion rate of the black hole only if the stars exhibit high wind massloss rates that are comparable with those of evolved 7-10 Myr old stars with masses of M = 19 − 25 M ⊙ . This is in contrast with observations that have shown that these stars are rather young, main-sequence B-stars. We therefore conclude that the S-stars cannot account for the accretion rate alone.

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“…2. For details about how to use AMUSE we refer the reader to Portegies Zwart et al (2013) and Pelupessy et al (2013). More information can be also found at http://amusecode.org.…”

Section: The Amuse Frameworkmentioning

confidence: 99%

Radial migration of the Sun in the Milky Way: a statistical study

Martínez-Barbosa

Brown

Zwart

2014

Monthly Notices of the Royal Astronomical Society

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The determination of the birth radius of the Sun is important to understand the evolution and consequent disruption of the Sun's birth cluster in the Galaxy. Motivated by this fact, we study the motion of the Sun in the Milky Way during the last 4.6 Gyr in order to find its birth radius. We carried out orbit integrations backward in time using an analytical model of the Galaxy which includes the contribution of spiral arms and a central bar. We took into account the uncertainty in the parameters of the Milky Way potential as well as the uncertainty in the present day position and velocity of the Sun. We find that in general the Sun has not migrated from its birth place to its current position in the Galaxy (R ). However, significant radial migration of the Sun is possible when: 1) The 2 : 1 Outer Lindblad resonance of the bar is separated from the corrotation resonance of spiral arms by a distance ∼ 1 kpc. 2) When these two resonances are at the same Galactocentric position and further than the solar radius. In both cases the migration of the Sun is from outer regions of the Galactic disk to R , placing the Sun's birth radius at around 11 kpc. We find that in general it is unlikely that the Sun has migrated significantly from the inner regions of the Galactic disk to R .

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The Astrophysical Multipurpose Software Environment

Cited by 209 publications

References 68 publications

On the formation of hot and warm Jupiters via secular high-eccentricity migration in stellar triples

On the formation of hot and warm Jupiters via secular high-eccentricity migration in stellar triples

Stellar winds near massive black holes – the case of the S-stars

Radial migration of the Sun in the Milky Way: a statistical study

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