Irreversibility in Small Stellar Dynamical Systems.

Miller, Richard H.

doi:10.1086/147911

Cited by 165 publications

(107 citation statements)

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“…We focused on the amplitudes of the Cartesian components of the variational vectors, X i ¼ ðX i ; Y i ; Z i Þ, since the variational velocities tend to exhibit spikes in their time dependence (Miller 1964). We examined three choices for the amplitude D of the separation: 1.…”

Section: Methodsmentioning

confidence: 99%

Instability of the GravitationalN‐Body Problem in the Large‐NLimit

Hemsendorf

Merritt

2002

ApJ

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Section: Methodsmentioning

confidence: 99%

Instability of the GravitationalN‐Body Problem in the Large‐NLimit

Hemsendorf

Merritt

2002

ApJ

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“…Although all orbits in an N-body system are mildly chaotic (e.g. , Miller 1964;Hemsendorf & Merritt 2002),for the purpose of testing our automated classification scheme, we also attempt to visually classify chaotic orbits, although this is not possible to do in a robust manner. An orbit was visually classified as chaotic only if it could not be easily identified with a major orbit family (box, short-axis tube, long-axis tube), or if it showed signs of changing from one family to another during the integration time (indicating that it is sticky chaotic).…”

Section: Orbit Classificationmentioning

confidence: 99%

A Unified Framework for the Orbital Structure of Bars and Triaxial Ellipsoids

Valluri

Shen

Abbott

et al. 2016

ApJ

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We examine a large random sample of orbits in two self-consistent simulations of N-body bars. Orbits in these bars are classified both visually and with a new automated orbit classification method based on frequency analysis. The well-known prograde x1 orbit family originates from the same parent orbit as the box orbits in stationary and rotating triaxial ellipsoids. However, only a small fraction of bar orbits (∼4%) have predominately prograde motion like their periodic parent orbit. Most bar orbits arising from the x1 orbit have little net angular momentum in the bar frame, making them equivalent to box orbits in rotating triaxial potentials. In these simulations a small fraction of bar orbits (∼7%) are long-axis tubes that behave exactly like those in triaxial ellipsoids: they are tipped about the intermediateaxis owingto the Coriolis force, with the sense of tipping determined by the sign of their angular momentum about the long axis. No orbits parented by prograde periodic x2 orbits are found in the pure bar model, but a tiny population (∼2%) of short-axis tube orbits parented by retrograde x4 orbits are found. When a central point mass representing a supermassive black hole (SMBH) is grown adiabatically at the center of the bar, those orbits that lie in the immediate vicinity of the SMBH are transformed into precessing Keplerian orbits thatbelong to the same major families (short-axis tubes, long-axis tubes and boxes) occupying the bar at larger radii. During the growth of an SMBH,the inflow of mass and outward transport of angular momentum transformsome x1 and long-axis tube orbits into prograde short-axis tubes. This study has important implications for future attempts to constrain the masses of SMBHs in barred galaxies using orbit-based methods like the Schwarzschild orbit superposition scheme and for understanding the observed features in barred galaxies.

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“…Such "parallel" calculations were used to study reversibility in n-body calculations earlier (Miller, 1964).…”

Section: Cn)mentioning

confidence: 99%

“…This definition also seems preferable because it is free of some of the complications of interpretation that go with explicit evaluations of 'IT ~ <J II (See, for example, Miller, 1964). …”

mentioning

confidence: 99%

Icr Quarterly Report Number 26.

Ashenhurst¹

1970

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Irreversibility in Small Stellar Dynamical Systems.

Cited by 165 publications

References 0 publications

Instability of the GravitationalN‐Body Problem in the Large‐NLimit

Instability of the GravitationalN‐Body Problem in the Large‐NLimit

A Unified Framework for the Orbital Structure of Bars and Triaxial Ellipsoids

Icr Quarterly Report Number 26.

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