Piet Hut

Massachusetts Institute of Technology

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Junichiro Makino

Tokyo Metropolitan Bokutoh Hospital

Michele Trenti

University of Melbourne

Douglas C. Heggie

Maxwell Institute for Mathematical Sciences

J. F. Traub

Columbia University

Stephen L. W. McMillan

Drexel University

Simon Portegies Zwart

Leiden University

Richard A. Muller

University of California, Berkeley

Holger Baumgardt

University of Queensland

Marc Davis

University of California, Berkeley

James B. Hartle

University of California, Santa Barbara

Cooperative Institutions

The University of Tokyo

California Institute of Technology

Princeton University

Max Planck Society

Center for Astrophysics Harvard & Smithsonian

Kyoto University

Netherlands Institute for Radio Astronomy

Massachusetts Institute of Technology

University of California, Santa Barbara

University of Cambridge

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Constraints on massive black holes as dark matter candidates

Monthly Notices of the Royal Astronomical Society (1992)

Piet Hut M. J. Rees

If our Galactic halo were composed of black holes as massive as 106 M⊙, then dynamical friction would have caused ∼ 100 such objects to settle toward the Galactic Center. Several processes can then ensue: slingshot effects, gravitational radiation induced coalescence, and possible 'loss cone' depletion of stars orbiting very close to the Galactic Center. The most likely outcome would be the accumulation of a central mass of ≫ 106 M⊙, much larger than is compatible with observations. These considerations strongly argue against the hypothesis that the halo is made of 106-M⊙ hole.

Black hole (networking)

Coalescence (physics)

Primordial black hole

10.1093/mnras/259.1.27p

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Citations (39)

Cometary showers and unseen solar companions (reply)

Nature (1984)

Richard A. Muller Piet Hut Marc Davis Walter Álvarez

10.1038/312380b0

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Citations (3)

Gravitational Thermodynamics

arXiv (Cornell University) (1997)

Piet Hut

The gravitational N-body problem, for $N>2$, is the oldest unsolved problem in mathematical physics. Some of the most ideal examples that can be found in nature are globular star clusters, with $N \sim 10^6$. In this overview, I discuss six types of fundamental sources of unpredictability, each of which poses a different challenge to attempts to determine the long-term behavior of these systems, governed by a peculiar type of thermodynamics.

10.48550/arxiv.astro-ph/9704286

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Star cluster ecology -- IV. Dissection of an open star cluster: photometry

Monthly Notices of the Royal Astronomical Society (2001)

Simon Portegies Zwart Stephen L. W. McMillan Piet Hut Junichiro Makino

The evolution of star clusters is studied using N-body simulations in which the evolution of single stars and binaries is taken self-consistently into account. Initial conditions are chosen to represent relatively young Galactic open clusters, such as the Pleiades, Praesepe and the Hyades. The calculations include a realistic mass function, primordial binaries and the external potential of the parent Galaxy.

Pleiades

Initial mass function

10.1046/j.1365-8711.2001.03976.x

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Citations (335)

Star clusters with primordial binaries - III. Dynamical interaction between binaries and an intermediate-mass black hole

Monthly Notices of the Royal Astronomical Society (2006)

Michele Trenti Eliani Ardi Shin Mineshige Piet Hut

We present the first study of the dynamical evolution of an isolated star cluster that combines a significant population of primordial binaries with the presence of a central black hole. We use equal-mass direct N-body simulations, with N ranging from 4096 to 16384 and a primordial binary ratio of 0-10%; the black hole mass is about one percent of the total mass of the cluster. The evolution of the binary population is strongly influenced by the presence of the black hole, which gives the cluster a large core with a central density cusp. Starting from a variety of initial conditions (Plummer and King models), we first encounter a phase, that last approximately 10 half-mass relaxation times, in which binaries are disrupted faster compared to analogous simulations without a black hole. Subsequently, however, binary disruption slows down significantly, due to the large core size. The dynamical interplay between the primordial binaries and the black hole thus introduces new features with respect to the scenarios investigated so far, where the influence of the black hole and of the binaries have been considered separately. A large core to half mass radius ratio appears to be a promising indirect evidence for the presence of a intermediate-mass black hole in old globular clusters.

Mass segregation

Black hole (networking)

Mass ratio

Primordial black hole

10.1111/j.1365-2966.2006.11189.x

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Citations (75)

A constraint on the distance dependence of the gravitational constant

Physics Letters B (1981)

Piet Hut

Yukawa potential

Gravitational constant

Newtonian potential

10.1016/0370-2693(81)90974-6

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Citations (27)

Cosmological tests of general relativity

Nature (1977)

Piet Hut

Scale factor (cosmology)

Cosmological constant

10.1038/267128a0

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Citations (3)

Varieties of limits to scientific knowledge

Complexity (1998)

Piet Hut David Ruelle J. F. Traub

for Advanced Study in Princeton.While his main research area is theoretical astrophysics, he is frequently invovled in multidisciplinary collaborations, from geology, paleontology and cognitive science to particle physics and computer science.He is currently involved in a Tokyo-based project aimed at developing a special purpose computer for simulations in stellar dynamics, with a speed of 1 Petaflops.

Columbia university

Natural science

10.1002/(sici)1099-0526(199807/08)3:6<33::aid-cplx5>3.3.co;2-c

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Citations (1)

Few-body modes of binary formation in core collapse

Astronomy and Computing (2013)

Ataru Tanikawa Douglas C. Heggie Piet Hut Junichiro Makino

10.1016/j.ascom.2013.11.002

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Citations (5)

Stability of tidal equilibrium

A&A (1980)

Piet Hut

Source

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Citations (61)