The Monte Carlo Method
By John R. Howell, M. Pinar Mengüç, K. Daun, Robert Siegel. Thermal Radiation Heat Transfer, 2020
327 citations recorded by the source corpus.
. This paper consists of two independent parts. (1) The Monte Carlo method for computing the evolution of spherical stellar systems has been modified so that the computation can be continued after the time of formation of the central singularity. Results are presented for systems with equal and unequal star masses. The initial core-halo formation is followed by a general expansion of the cluster, while the central singularity absorbs a growing fraction of the total negative energy. (2) Theoretical expressions of the 'diffusion coefficients', which describe the effect of encounters in a stellar system, contain a factor \n(yN) where TV is the number of stars and y is a constant usually taken to be of the order of 0.4. A reconsideration of the 'non-dominant terms' leads to a substantially lower value, of the order of 0.15 for equal masses and 0.075 for unequal masses with a typical distribution. • This correction improves the agreement between JV-body and Monte Carlo simulations of spherical systems.
Subfields: Condensed Matter Physics, Numerical Analysis, Statistics and Probability
View Paper: https://www.semanticscholar.org/paper/6bd56038967a3dd890d12f63198f5ba1b46f4a98
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Citations in the corpus
- Recovery of Graded Response Model Parameters (2012, methodology): “In practice, the joint posteriors of complex models are analytically intractable, and Markov chain Monte Carlo (MCMC) methods (Hastings, 1970; Metropolis, Rosenbluth, Rosenbluth, Teller, & Teller, 1953; Metropolis & Ulam, 1949) are used to simulate draws from the posterior.”