Tidal interactions in star cluster simulations

By Rosemary A. Mardling, S. Aarseth. 2001

365 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/9d58acd85ceb2c7b8f76e55cc9b9c4982af4ac04

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In Astronomy and Astrophysics

1. S. Naoz
2. F. Antonini
3. F. Rasio
4. B. Kocsis
5. S. Toonen
6. Joseph M. Antognini
7. T. Thompson
8. C. Rodriguez

In Statistical and Nonlinear Physics

1. S. Naoz
2. S. Aarseth
3. F. Rasio
4. S. Toonen
5. C. Tout
6. J. Hurley
7. F. Antonini
8. S. P. Portegies Zwart

Citations in the corpus

• The Eccentric Kozai-Lidov Effect and Its Applications (2016, background): “ to the condition in Equation (50). Another consequence of large eccentricities is the stability of the system. A long term stability condition that is often used in the literature is the one give by Mardling and Aarseth (2001), which has the following form a 2 a 1 >2:8 1 + m 3 m 1 + m 2 2=5 (1”
• ON THE TRIPLE ORIGIN OF BLUE STRAGGLERS (2009, methodology): “…simulation of the evolution of primordial triples drawn from appropriate distributions (as described in Fabrycky & Tremaine 2007, where all inner binaries were assumed to have initial periods ofP > 6 days) and the triples were checked for stability using the criterion of Mardling & Aarseth (2001).”
• Binary Black Hole Mergers from Field Triples: Properties, Rates, and the Impact of Stellar Evolution (2017, methodology): “The rest of the systems became dynamically unstable (Mardling & Aarseth 2001) during their evolution due to e.g. stellar wind mass loss (Perets & Kratter 2012) and supernova kicks.”
• The Kozai Mechanism and the Evolution of Binary Supermassive Black Holes (2002, methodology): “We adopt as a stability criterion the empirical formula used by Mardling & Aarseth (2001), which may be written as a2 a1 > 2.8 1− e2 [( 1 + m2 m0 +m1 ) 1 + e2 (1− e2)1/2 ]2/5 .”
• Stellar collisions during binary–binary and binary–single star interactions (2004, methodology): “For the case of a hierarchical quadruple composed of two binaries (‘[[• •] [• •]]’ in Table 2), FEWBODY uses the additional correction factor presented in section 4.2 of Mardling & Aarseth (2001).”
• BLACK HOLE TRIPLE DYNAMICS: A BREAKDOWN OF THE ORBIT AVERAGE APPROXIMATION AND IMPLICATIONS FOR GRAVITATIONAL WAVE DETECTIONS (2013, methodology): “…that satisfy the stability criterion (e.g., Blaes et al. 2002; Wen 2003; Fabrycky & Tremaine 2007; Hamers et al. 2013): a2 a1 > 3.3 1− e2 [ 2 3 ( 1 + m2 Mb ) 1 + e2 (1− e2)1/2 ]2/5 (11) ×(1− 0.3I/π) , which was derived in Mardling & Aarseth (2001) by means of Newtonian direct N−body simulations.”
• ON THE FORMATION OF HOT JUPITERS IN STELLAR BINARIES (2012, background): “We have found that the results were essentially unaffected. that all our initial conditions are stable according to the Mardling & Aarseth (2001) criterion.”
• BLACK HOLE MERGERS AND BLUE STRAGGLERS FROM HIERARCHICAL TRIPLES FORMED IN GLOBULAR CLUSTERS (2015, neutral): “In what follows we only consider triple systems that satisfy the stability criterion of Mardling & Aarseth (2001), a2 a1 > 3.3 1− e2 [ 2 3 ( 1 + m2 Mb ) 1 + e2 (1− e2)1/2 ]2/5 (1) ×(1− 0.3I/π) , with Mb = m0 +m1.”
• Dynamics of triple black hole systems in hierarchically merging massive galaxies (2006, background): “Mardling & Aarseth (2001) derive a criterion for the stability of 3-body systems based on an analogue with the problem of binary tides.”
• RESONANT POST-NEWTONIAN ECCENTRICITY EXCITATION IN HIERARCHICAL THREE-BODY SYSTEMS (2012, methodology): “We also show two stability criteria, ǫ = 0.1, dotted magenta lines and the Mardling & Aarseth (2001) criterion [Eq.”
• Suppression of extreme orbital evolution in triple systems with short-range forces (2014, background): “These conditions of parameters are subject to the stability criterion of Mardling & Aarseth (2001) a2 a1 > 2.8 ( 1 + m2 m0 )2/5 (1 + e2) 2/5 (1− e2)6/5 ( 1− 0.3itot 180◦ ) .”
• A complete N-body model of the old open cluster M67 (2005, methodology): “Binary orbits may also become chaotic owing to perturbations from nearby stars and this scenario is modelled using the Mardling & Aarseth (2001) algorithm.”
• Formation and Evolution of Compact-object Binaries in AGN Disks (2019, background): “If the angle between the inner and outer orbits becomes ∼90° after inner binary–single interactions and a third body is stably bound after the interactions (Mardling & Aarseth 2001), mergers can be driven by the KL mechanism.”
• Eccentric Black Hole Mergers in Dense Star Clusters: The Role of Binary–Binary Encounters (2018, methodology): “We determine if a triple is stable according to the stability criterion from Mardling & Aarseth (2001): a1(1 − e1) a11 > 2.8 [( 1 + m11 m12 ) 1 + e1√ 1 − e1 ]2/5( 1 − 0.3i π ) (6) where i is the inclination of the outer component’s orbit relative to the orbital plane of the inner binary and once we…”
• Secular Evolution of Hierarchical Planetary Systems (2002, methodology): “The stability of the HD 168443 system is consistent with the empirical stability criteria for hierarchical triple systems derived most recently by Eggleton & Kiseleva (1995) and Mardling & Aarseth (2001).”
• FROM BINARIES TO MULTIPLES. II. HIERARCHICAL MULTIPLICITY OF F AND G DWARFS (2014, background): “For example, the stability criterion of Mardling & Aarseth (2001) for co-planar orbits can be written as PL/PS > 4.7(1− eL)−1.8(1 + eL)0.6(1 + qout)0.1, (3) where eL is the eccentricity of the outer orbit, while the ratio of the distant-companion mass to the combined mass of the inner binary qout…”