Integral Dynamical Models in Mathematical Ecology

1996 ◽  
pp. 27-34
Author(s):  
Natali Hritonenko ◽  
Yuri Yatsenko
Keyword(s):  
Mathematical Ecology ◽  
Dynamical Models

Diagnosing Chaos in the Logistic Family of Discrete Market Dynamical Models

2003 ◽  
Author(s):  
Brynn Hibbert ◽  
Jixiu Jiang ◽  
Ian Wilkinson
Keyword(s):  
Dynamical Models ◽  
Logistic Family

Improved Evidence for a Black Hole in M32 fromHST/FOS Spectra. II. Axisymmetric Dynamical Models

1998 ◽  
Vol 493 (2) ◽  
pp. 613-631 ◽  
Author(s):  
Roeland P. van der Marel ◽  
N. Cretton ◽  
P. Tim de Zeeuw ◽  
Hans‐Walter Rix
Keyword(s):  
Black Hole ◽  
Dynamical Models

scholarly journals Precipitation downscaling under climate change: Recent developments to bridge the gap between dynamical models and the end user

2010 ◽  
Vol 48 (3) ◽  
Author(s):  
D. Maraun ◽  
F. Wetterhall ◽  
A. M. Ireson ◽  
R. E. Chandler ◽  
E. J. Kendon ◽  
...  
Keyword(s):  
Climate Change ◽  
End User ◽  
Dynamical Models ◽  
Recent Developments

scholarly journals The geometric structures and instability of entropic dynamical models

2011 ◽  
Vol 227 (1) ◽  
pp. 459-471 ◽  
Author(s):  
Linyu Peng ◽  
Huafei Sun ◽  
Dandi Sun ◽  
Jin Yi
Keyword(s):  
Dynamical Models ◽  
Geometric Structures

scholarly journals Anisotropy in ω Centauri and 47 Tucanae

1988 ◽  
Vol 126 ◽  
pp. 663-664
Author(s):  
G. Meylan
Keyword(s):  
Globular Clusters ◽  
Velocity Dispersion ◽  
Dynamical Models ◽  
Comprehensive Description ◽  
Great Opportunity ◽  
The Galaxy

The southern sky gives us the great opportunity to observe two among the brightest and nearest globular clusters of the Galaxy: ω Cen and 47 Tuc. For these giant clusters, we present the comparison between observations and King-Michie multi-mass dynamical models with anisotropy in the velocity dispersion. A more comprehensive description of this work is to be published (Meylan 1986a,b).

scholarly journals A signed network perspective on the government formation process in parliamentary democracies

2021 ◽  
Vol 11 (1) ◽  
Author(s):  
Angela Fontan ◽  
Claudio Altafini
Keyword(s):  
Decision Making ◽  
Formation Process ◽  
Signed Graph ◽  
Balance Theory ◽  
Collective Decision Making ◽  
Dynamical Models ◽  
Average Correlation ◽  
Parliamentary Democracies ◽  
Signed Network ◽  
The Government

AbstractIn parliamentary democracies, government negotiations talks following a general election can sometimes be a long and laborious process. In order to explain this phenomenon, in this paper we use structural balance theory to represent a multiparty parliament as a signed network, with edge signs representing alliances and rivalries among parties. We show that the notion of frustration, which quantifies the amount of “disorder” encoded in the signed graph, correlates very well with the duration of the government negotiation talks. For the 29 European countries considered in this study, the average correlation between frustration and government negotiation talks ranges between 0.42 and 0.69, depending on what information is included in the edges of the signed network. Dynamical models of collective decision-making over signed networks with varying frustration are proposed to explain this correlation.

scholarly journals What to expect when using globular clusters as tracers of the total mass distribution in Milky Way-mass galaxies

2021 ◽  
Vol 502 (2) ◽  
pp. 2828-2844
Author(s):  
Meghan E Hughes ◽  
Prashin Jethwa ◽  
Michael Hilker ◽  
Glenn van de Ven ◽  
Marie Martig ◽  
...  
Keyword(s):  
Dark Matter ◽  
Radial Distribution ◽  
Globular Clusters ◽  
Dominant Factor ◽  
Quality Uncertainty ◽  
Dynamical Models ◽  
Accuracy And Precision ◽  
The Galaxy ◽  
Dark Matter Distribution ◽  
Ideal Tracer

ABSTRACT Dynamical models allow us to connect the motion of a set of tracers to the underlying gravitational potential, and thus to the total (luminous and dark) matter distribution. They are particularly useful for understanding the mass and spatial distribution of dark matter (DM) in a galaxy. Globular clusters (GCs) are an ideal tracer population in dynamical models, since they are bright and can be found far out into the halo of galaxies. We aim to test how well Jeans-Anisotropic-MGE (JAM) models using GCs (positions and line-of-sight velocities) as tracers can constrain the mass and radial distribution of DM haloes. For this, we use the E-MOSAICS suite of 25 zoom-in simulations of L* galaxies. We find that the DM halo properties are reasonably well recovered by the JAM models. There is, however, a strong correlation between how well we recover the mass and the radial distribution of the DM and the number of GCs in the galaxy: the constraints get exponentially worse with fewer GCs, and at least 150 GCs are needed in order to guarantee that the JAM model will perform well. We find that while the data quality (uncertainty on the radial velocities) can be important, the number of GCs is the dominant factor in terms of the accuracy and precision of the measurements. This work shows promising results for these models to be used in extragalactic systems with a sample of more than 150 GCs.

scholarly journals A Precise Benchmark for Cluster Scaling Relations: Fundamental Plane, Mass Plane and IMF in the Coma Cluster from Dynamical Models

2020 ◽  
Author(s):  
Shravan Shetty ◽  
Michele Cappellari ◽  
Richard M McDermid ◽  
Davor Krajnović ◽  
P T de Zeeuw ◽  
...  
Keyword(s):  
Galaxy Formation ◽  
Scaling Relations ◽  
Coma Cluster ◽  
Dynamical Models ◽  
Fundamental Plane ◽  
Cluster Galaxies ◽  
Dynamical Scaling ◽  
Small Uncertainty ◽  
Cluster Distance ◽  
Using Data

Abstract We study a sample of 148 early-type galaxies in the Coma cluster using SDSS photometry and spectra, and calibrate our results using detailed dynamical models for a subset of these galaxies, to create a precise benchmark for dynamical scaling relations in high-density environments. For these galaxies, we successfully measured global galaxy properties, modeled stellar populations, and created dynamical models, and support the results using detailed dynamical models of 16 galaxies, including the two most massive cluster galaxies, using data taken with the SAURON IFU. By design, the study provides minimal scatter in derived scaling relations due to the small uncertainty in the relative distances of galaxies compared to the cluster distance. Our results demonstrate low (≤55% for 90th percentile) dark matter fractions in the inner 1Re of galaxies. Owing to the study design, we produce the tightest, to our knowledge, IMF-σe relation of galaxies, with a slope consistent with that seen in local galaxies. Leveraging our dynamical models, we transform the classical Fundamental Plane of the galaxies to the Mass Plane. We find that the coefficients of the mass plane are close to predictions from the virial theorem, and have significantly lower scatter compared to the Fundamental plane. We show that Coma galaxies occupy similar locations in the (M* - Re) and (M* - σe) relations as local field galaxies but are older. This, and the fact we find only three slow rotators in the cluster, is consistent with the scenario of hierarchical galaxy formation and expectations of the kinematic morphology-density relation.

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