arXiv subjects

Jae Woo Lee

Publications and source records attributed to Jae Woo Lee.

At least 37 records · Page 2Linked to original sources

arXiv2022

V608 Cassiopeiae: A W UMa-type eclipsing binary with two possible circumbinary companions

We present the photometric properties of V608 Cas from detailed studies of light curves and eclipse timings. The light curve synthesis indicates that the eclipsing pair is an overcontact binary with parameters of $ΔT$ = 155 K, $q$ = 0.328, and $f$ = 26 %. We detected the third light $\ell_{3}$, which corresponds to about 8 % and 5 % of the total systemic light in $V$ and $R$ bands, respectively. Including our 6 timing measurements, a total of 38 times of minimum light were used for a period study. It was found that the orbital period of V608 Cas has varied in some combination of an upward parabola and two periodic variations. The continuous period increase with a rate of $+$3.99$\times$10$^{-7}$ d yr$^{-1}$ can be interpreted as a mass transfer from the secondary component to the primary star at a rate of 1.51$\times$10$^{-7}$ M$_\odot$ yr$^{-1}$. The periods and semi-amplitudes of the two periodic variations are about $P_3$ = 16.0 yr and $P_4$ = 26.3 yr, and $K_3$ = 0.0341 d and $K_4$ = 0.0305 d, respectively. The most likely explanation of both cycles is a pair of light-traveling time effects operated by the possible presence of third and fourth components with estimated masses of $M_3$ = 2.20 M$_\odot$ and $M_4$ = 1.27 M$_\odot$ in eccentric orbits of $e_3$ = 0.66 and $e_4$ = 0.52. Because the contribution of $\ell_{3}$ is very low compared to the estimated masses of two circumbinary objects, they can be inferred as very faint compact objects.

astro-ph.SR↗

arXiv2022

The Pre-He White Dwarfs in Eclipsing Binaries. III. WASP 1625-04

1SWASP J162545.15-043027.9 (WASP 1625-04) has been announced as one of EL CVn candidates showing total primary eclipses and ellipsoidal variations. This paper presents the absolute properties of the binary star, based on our high-resolution spectroscopy conducted from 2015 through 2020. From the spectral analysis, the radial velocities (RVs) for both components were obtained with the effective temperature $T_{\rm eff,1} = 8990 \pm 200$ K and the rotational rate $v_1\sin$$i=53\pm5$ km s$^{-1}$ for the more massive primary. The RV measurements were analyzed with archival WASP photometry. From the modelling we obtained: $M_1 = 1.745 \pm 0.013$ M$_\odot$, $M_2 = 0.187 \pm 0.002$ M$_\odot$, $R_1 = 1.626 \pm 0.008$ M$_\odot$, $R_2 = 0.290 \pm 0.003$ M$_\odot$, $L_1 = 15.5 \pm 1.4$ L$_\odot$, and $L_2 = 1.84 \pm 0.16$ L$_\odot$. In the Hertzsprung-Russell diagram, WASP 1625-04 A lies on the zero-age main sequence and its companion accords well with the helium-core white dwarf models of 0.19 M$_\odot$ in the constant luminosity phase. Our improved results demonstrate that WASP 1625-04 is a typical EL CVn-type binary with a low mass ratio and $M_2$ combination in the thin-disk population and is the product of the stable, non-conservative mass transfer of the precursor binary.

astro-ph.SR↗

arXiv2021

TESS Eclipsing Binary Stars. I. Short cadence observations of 4584 eclipsing binaries in Sectors 1-26

In this paper we present a catalog of 4584 eclipsing binaries observed during the first two years (26 sectors) of the TESS survey. We discuss selection criteria for eclipsing binary candidates, detection of hither-to unknown eclipsing systems, determination of the ephemerides, the validation and triage process, and the derivation of heuristic estimates for the ephemerides. Instead of keeping to the widely used discrete classes, we propose a binary star morphology classification based on a dimensionality reduction algorithm. Finally, we present statistical properties of the sample, we qualitatively estimate completeness, and discuss the results. The work presented here is organized and performed within the TESS Eclipsing Binary Working Group, an open group of professional and citizen scientists; we conclude by describing ongoing work and future goals for the group. The catalog is available from http://tessEBs.villanova.edu and from MAST.

astro-ph.SR↗

arXiv2021

Pulsation and Rotation of the EL CVn-type Eclipsing Binary 1SWASP J024743.37-251549.2

EL CVn-type eclipsing binaries are composed of a massive A-type main-sequence primary star and a hotter B-type secondary star. This paper presents the time-series photometric and asteroseismic results of the EL CVn-type star 1SWASP J024743.37-251549.2. Well-defined eclipsing light curves were constructed by using the novel high-cadence $BV$ data and archival {\it TESS} data, and the physical parameters of each binary component were derived by modeling the light curves. Multiple frequency analysis was performed to investigate the pulsation properties of the binary components. A reliable signal could not be detected in the high-frequency region of 100--300 day$^{-1}$, unlike in the previous discovery of three frequencies around 200 day$^{-1}$. This indicates that the pulsation amplitudes of the pre-helium white dwarf secondary component decreased considerably. By contrast, 12 frequencies were detected in the range of 33 to 53 day$^{-1}$. Most of them were classified as $δ$ Sct-type pulsations originating from the primary star. Theoretical frequencies for the seismic analysis were obtained by adding the non-rotating model frequencies from the GYRE and their rotational shifts from the complete calculation approach. Grid-based fitting was conducted for various stellar properties. The theoretical frequencies and stellar parameters of the best solution concurred well with the observations. The rotation rate was constrained to 1.50 $\pm$ 0.02 day$^{-1}$, indicating the synchronized rotation of the primary star. The results imply that the complete approach based on the polytropic model is applicable to the seismic analysis of fast-rotating $δ$ Sct stars.

astro-ph.SR↗

arXiv2021

Tidally Perturbed Oblique Pulsations in the Hierarchical Triple System V1031 Orionis

We present TESS photometry of the triple star system V1031 Ori (AB)C, which exhibits short-period oscillations superimposed on an eclipsing light curve. The high-quality data were analyzed in detail and combined with the published spectroscopic measurements to obtain the fundamental stellar parameters of the program target. The masses and radii of the eclipsing pair (AB) were determined to about 0.5 \% and 0.7 \% precision, respectively. We found 23 significant frequencies in two ranges of $<$ 2 day$^{-1}$ and 10.9$-$12.7 day$^{-1}$ from the eclipse-subtracted residuals. Among them, sixteen in the gravity ($g$)-mode region may be aliases and artefacts due to imperfect removal of the systematic trends and the binary effects from the TESS data. Seven frequencies in the pressure ($p$)-mode region were separated by the orbital frequency and split by the average offset of 0.042 $\pm$ 0.003 day$^{-1}$ from their adjacent harmonics. Further, the pulsation amplitudes are clearly modulated with the binary star orbit. The results indicate that the $p$-mode frequencies are tidally perturbed pulsations from the secondary component and the pulsation axis could be aligned with the tidal axis.

astro-ph.SR↗

arXiv2020

Tidally Excited Modes and $δ$ Scuti Pulsations in the Eclipsing Triple Star IM Persei

IM Per is a triple star system whose eclipsing pair masses and radii are accurate to within 1 \%. The TESS light curve of the program target exhibits partial eclipses and multiple oscillations with mmag-level amplitudes. It is found that the oscillations affect eclipse timing measurements. Binary modeling of the high-quality TESS data indicates that the eclipsing components of the triple system are twin dwarfs with parameters of $M_2$/$M_1$ = 0.995, $R_2$/$R_1$ = 0.901, and $Δ$($T_{\rm eff,1}$--$T_{\rm eff,2}$) = 12 K in an eccentric ($e$ = 0.049), detached configuration. The third light of $l_3$ = 0.054 may mostly come from a G-type tertiary companion. Our predicted parallax of 1.52 $\pm$ 0.09 mas is concurrent with the Gaia measurement of 1.52 $\pm$ 0.05 mas. Multifrequency analysis of the outside-eclipse residuals reveals 22 significant pulsation signals: four in the gravity-mode region (0.03$-$2.22 day$^{-1}$) and 18 in the pressure-mode region (9.19$-$25.12 day$^{-1}$). Of the low frequencies, $f_{11}$ and $f_{14}$ are orbital harmonics that can be identified as tidally excited modes. The pulsation periods and constants for the high frequencies, and the position in the Cepheid instability strip demonstrate that the pulsating component of IM Per is a $δ$ Sct variable.

astro-ph.SR↗

arXiv2020

$β$ Cephei Pulsations in the High-mass Eclipsing System CW Cephei

CW Cep is an early B-type eclipsing binary with mass measurement precisions better than 1 \%. We report the discovery of pulsation signatures in the TESS time-series data of the system observed during Sectors 17 and 18. Our binary modeling indicates that the target star is a partially-eclipsing detached system with masses of 12.95 $M_\odot$ and 11.88 $M_\odot$ and radii of 5.52 $R_\odot$ and 5.09 $R_\odot$ in an eccentric orbit of $e$ = 0.0305. The distance to the eclipsing system, 928 $\pm$ 36 pc, is much more precise than the Gaia distance of 962 $\pm$ 453 pc. Applying multifrequency analyses to the residual light curve in the outside-eclipse part, we detected 13 significant signals in two frequency regions. Six frequencies below 1 day$^{-1}$ appeared to be mostly orbital harmonic and combination terms, or sidelobes due to insufficient removal of the binary effects. In contrast, seven frequencies clustered around 2.73 day$^{-1}$ and 5.34 day$^{-1}$ could be considered $β$ Cep-type pulsations. Our results represent the second discovery of $β$ Cep pulsations present in double-lined eclipsing binaries with precise masses and, hence, CW Cep serves as an important test-bed for the asteroseismic modeling of high-mass stars.

astro-ph.SR↗

arXiv2020

Physical Nature of the Eclipsing δ Scuti Star AO Serpentis

We present the absolute properties of the eclipsing binary AO Ser with a pulsating component from our $BV$ photometric and high-resolution spectroscopic observations, which were performed between April and May 2017. The radial velocities (RVs) for both components were measured, and the effective temperature and projected rotational velocity of the primary star were determined to be $T_{\rm eff,1}$ = 8,820 $\pm$ 62 K and $v_1 \sin i_{1}$ = 90 $\pm$ 18 km s$^{-1}$, respectively, by comparing the observed spectrum with the Kurucz models. The accurate fundamental parameters of AO Ser were determined by a simultaneous analysis of the light and RV curves. The masses and radii of the primary and secondary components are $M_1$ = 2.55 $\pm$ 0.09 M$_\odot$ and $R_1$ = 1.64 $\pm$ 0.02 R$_\odot$ and $M_2$ = 0.49 $\pm$ 0.02 M$_\odot$ and $R_2$ = 1.38 $\pm$ 0.02 R$_\odot$, respectively. Multiple frequency analyses for the eclipse-subtracted light residuals were conducted. As a result, we detected two frequencies of $f_1$ = 21.852 days$^{-1}$ and $f_2$ = 23.484 days$^{-1}$. The evolutionary position on the HR diagram and the pulsational characteristics indicate that the primary star is a $δ$ Sct pulsator with a radial fundamental mode. On the other hand, the relatively evolved secondary is oversized for its own mass.

astro-ph.SR↗

arXiv2020

The Pre-He White Dwarfs in Eclipsing Binaries. I. WASP 0131+28

We report the first $BV$ light curves and high-resolution spectra of the post-mass transfer binary star WASP 0131+28 to study the absolute properties of extremely low-mass white dwarfs. From the observed spectra, the double-lined radial velocities were derived, and the effective temperature and rotational velocity of the brighter, more massive primary were found to be $T_{\rm eff,1} = 10,000 \pm 200$ K and $v_1\sin$$i$ = 55 $\pm$ 10 km s$^{-1}$, respectively. The combined analysis of the {\it TESS} archive data and ours yielded the accurate fundamental parameters of the program target. The masses were derived to about 1.0 \% accuracy and the radii to 0.6 \%, or better. The secondary component's parameters of $M_2 = 0.200 \pm 0.002$ M$_\odot$, $R_2 = 0.528 \pm 0.003$ R$_\odot$, $T_{\rm eff,2}$ = 11,186 $\pm$ 235 K, and $L_2 = 3.9 \pm 0.3$ L$_\odot$ are in excellent agreement with the evolutionary sequence for a helium-core white dwarf of mass 0.203 M$_\odot$, and indicates that this star is halfway through the constant luminosity phase. The results presented in this article demonstrate that WASP 0131+28 is an EL CVn eclipsing binary in a thin disk, which is formed from the stable Roche-lobe overflow channel and composed of a main-sequence dwarf with a spectral type A0 and a pre-He white dwarf.

astro-ph.SR↗

arXiv2020

Estimation of Infection Rate and Prediction of Initial Infected Individuals of COVID-19

We consider the pandemic spreading of COVID-19 for some selected countries after the outbreak of the coronavirus in Wuhan City, China. We estimated the infection rate and the initial infected individuals of COVID-19 by using the officially reported data at the early stage of the epidemic for the susceptible (S), infectable (I), quarantined (Q), and the cofirmed recovered (Rk) population model, so called SIQRk model. In the reported data we know the quarantined cases and the recovered cases. We can not know the recovered cases from the asymptomatic cases. In the SIQRk model we can estimated the model parameters and the initial infecting cases (confirmed ans asymtomatic cases) from the data fits. We obtained the infection rate in the range between 0.233 and 0.462, the basic reproduction number Ro in the range between 1.8 and 3.5, and the initial number of infected individuals in the range betwee 10 and 8409 for some selected countries. By using fitting parameters we estimated the maximum time of the infection for Germany when the government are performing the quarantine policy. The disease is undergoing to the calm state about six months after first patients were identified.

q-bio.PE↗

arXiv2020

TESS Photometry of the Eclipsing $δ$ Scuti Star AI Hydrae

AI Hya has been known as an eclipsing binary with a monoperiodic $δ$ Sct pulsator. We present the results from its {\it TESS} photometry observed during Sector 7. Including our five minimum epochs, the eclipse timing diagram displays the apsidal motion with a rate of $\dotω$ = 0.075$\pm$0.031 deg year$^{-1}$, which corresponds to an apsidal period of U = 4800$\pm$2000 years. The binary star model represents that the smaller, less massive primary component is 427 K hotter than the pulsating secondary, and our distance of 612$\pm$36 pc is in good agreement with the $Gaia$ distance of 644$\pm$26 pc. We subtracted the binary effects from the observed {\it TESS} data and applied a multifrequency analysis to these residuals. The result reveals that AI Hya is multiperiodic in its pulsation. Of 14 signals detected, four ($f_1$, $f_2$, $f_3$, $f_6$) may be considered independent pulsation frequencies. The period ratios of $P_{\rm pul}/P_{\rm orb}$ = 0.012$-$0.021 and the pulsation constants of $Q$ = 0.30$-$0.52 days correspond to $δ$ Sct pulsations in binaries. We found that the secondary component of AI Hya pulsates in both radial fundamental $F$ modes ($f_2$ and $f_3$) and non-radial $g_1$ modes with a low degree of $\ell$ = 2 ($f_1$ and $f_6$).

astro-ph.SR↗

arXiv2019

Absolute Properties of the Eclipsing $γ$ Dor Star V404 Lyrae

We present the first high-resolution spectra for the eclipsing binary V404 Lyr showing $γ$ Dor pulsations, which we use to study its absolute properties. By fitting models to the disentangling spectrum of the primary star, we found that it has an effective temperature of $T_{\rm eff,1}=7,330 \pm 150$ K and a rotational velocity of $v_1\sin$$i=148\pm18$ km s$^{-1}$. The simultaneous analysis of our double-lined radial velocities and the pulsation-subtracted ${\it Kepler}$ data gives us accurate stellar and system parameters of V404 Lyr. The masses, radii, and luminosities are $M_1$ = 2.17$\pm$0.06 M$_\odot$, $R_1$ = 1.91$\pm$0.02 R$_\odot$, and $L_1$ = 9.4$\pm$0.8 L$_\odot$ for the primary, and $M_2$ = 1.42$\pm$0.04 M$_\odot$, $R_2$ = 1.79$\pm$0.02 R$_\odot$, and $L_2$ = 2.9$\pm$0.2 L$_\odot$ for the secondary. The tertiary component orbiting the eclipsing pair has a mass of $M_{\rm 3b}$ = 0.71$\pm$0.15 $M_\odot$ in an orbit of $P_{\rm 3b}$ = 642$\pm$3 days, $e_{\rm 3b}$ = 0.21$\pm$0.04, and $a_{\rm 3b}$ = 509$\pm$2 R$_\odot$. The third light of $l_3=4.1\pm0.2\%$ could be partly attributable to the K-type circumbinary object. By applying a multiple frequency analysis to the eclipse-subtracted light residuals, we detected 45 frequencies with signal to noise amplitude ratios larger than 4.0. Identified as independent pulsation modes, seven frequencies ($f_1-f_6$, $f_9$), their new pulsation constants, and the location in the Hertzsprung-Russell diagram indicate that the pulsating primary is a $γ$ Dor-type variable star.

astro-ph.SR↗

arXiv2019

The Pulsating Eclipsing Binary TIC 309658221 in a 7.59 Day Orbit

We present a new eclipsing binary (EB) showing multiperiodic oscillations using the first three sectors of {\it TESS} photometry. The eclipse and pulsation light curves of TIC 309658221 were modeled using an iterative method to obtain a consistent photometric solution. The {\it TESS} target is a circular-orbit, detached binary system with a mass ratio of 0.349, an inclination angle of 80.42 deg, and a temperature difference of 847 K between the components. The primary component of the system lies near the red edge of the $δ$ Sct instability region on the main-sequence band in the Hertzsprung-Russell diagram. Multiple frequency analyses were applied to the eclipse-subtracted residuals after removing the binary effects in the observed data. These resulted in the detection of 26 frequencies, of which $f_1-f_6$ were independent pulsation frequencies. The 20 other frequencies could be mainly caused by orbital harmonics ($f_8$ and $f_{11}$) or combination frequencies. The period ratios and pulsation constants of the $f_1-f_6$ frequencies are in the ranges of $P_{\rm pul}/P_{\rm orb}$ = 0.010$-$0.013 and Q = 0.027$-$0.036 days, respectively, which are typical of $δ$ Sct type. The results reveal that TIC 309658221 is an eclipsing $δ$ Sct star with an orbital period of 7.5952 days and pulsation frequencies of 9.94$-$13.01 day$^{-1}$. This work demonstrates that the 2-min cadence observations of {\it TESS} are very useful for the study of pulsating EBs with multiple frequencies and low amplitudes.

astro-ph.SR↗

arXiv2019

Competition-induced increase of species abundance in mutualistic networks

Nutrients from a flowering plant are shared by its pollinators, giving rise to competition in the latter. Such exploitative competition of pollinators can limit their abundance and affect the global organization of the mutualistic partnership in the plant-pollinator mutualistic community. Here we investigate the effects of the exploitative competition between pollinators on the structure and the species abundance of the mutualistic networks which evolve by changing mutualistic partnership towards higher abundance of species. Simulations show different emergent network characteristics between plants and animals; hub plants connected to many pollinators are very rare while a few super-hub pollinators appear with the exploitative competition included, in contrast to equally many hubs of both types without the exploitative competition. More interestingly, the abundance of plant species increases with increasing the exploitative competition strength. We analyze the inverse of the generalized interaction matrix in the weak-interaction limit to identify the leading structural factors relevant to the species abundance, which are shown to be instrumental in optimizing the network structure to increase the mutualistic benefit and lower the cost of exploitative competition.

q-bio.PE↗

arXiv2018

The Eclipsing $δ$ Scuti Star EPIC 245932119

We present the physical properties of EPIC 245932119 ($K_{\rm p}$ = $+$9.82) exhibiting both eclipses and pulsations from the {\it K{\rm 2}} photometry. The binary modeling indicates that the eclipsing system is in detached or semi-detached configurations with a mass ratio of 0.283 or 0.245, respectively, and that its light-curve parameters are almost unaffected by pulsations. Multiple frequency analyses were performed for the light residuals in the outside-primary eclipsing phase after subtracting the binarity effects from the observed data. We detected 35 frequencies with signal to noise amplitude ratios larger than 4.0 in two regions of 0.62$-$6.28 day$^{-1}$ and 19.36$-$24.07 day$^{-1}$. Among these, it is possible that some high signals close to the Nyquist limit $f_{\rm Ny}$ may be reflections of real pulsation frequencies (2$f_{\rm Ny}-f_i$). All frequencies ($f_8$, $f_9$, $f_{14}$, $f_{18}$, $f_{24}$, $f_{32}$) in the lower frequency region are orbital harmonics, and three high frequencies ($f_{19}$, $f_{20}$, $f_{22}$) appear to be sidelobes split from the main frequency of $f_1$ = 22.77503 day$^{-1}$. Most of them are thought to be alias effects caused by the orbital frequency. For the 26 other frequencies, the pulsation periods and pulsation constants are in the ranges of 0.041$-$0.052 days and 0.013$-$0.016 days, respectively. These values and the position in the Hertzsprung-Russell diagram reveal that the primary component is a $δ$ Sct pulsator. The observational properties of EPIC 245932119 are in good agreement with those for eclipsing binaries with $δ$ Sct-type pulsating components.

astro-ph.SR↗

arXiv2018

KIC 6206751: the first R CMa-type eclipsing binary with $γ$ Doradus pulsations

We present the absolute properties of the double-lined eclipsing binary KIC 6206751 exhibiting multiperiodic pulsations. The ${\it Kepler}$ light curve of this system was simultaneously solved with the radial-velocity data given by Matson et al. (2017). The results indicate that the binary star is a short-period semi-detached system with fundamental parameters of $M_1$ = 1.66$\pm$0.04 M$_\odot$, $M_2$ = 0.215$\pm$0.006 M$_\odot$, $R_1$ = 1.53$\pm$0.02 R$_\odot$, $R_2$ = 1.33$\pm$0.02 R$_\odot$, $L_1$ = 5.0$\pm$0.6 L$_\odot$, and $L_2$ = 0.96$\pm$ 0.09 L$_\odot$. We applied multiple frequency analyses to the eclipse-subtracted light residuals and detected the 42 frequencies below 2.5 d$^{-1}$. Among these, three independent frequencies of $f_2$, $f_3$, and $f_4$ can be identified as high-order (38 $\le n \le$ 40) low-degree ($\ell$ = 2) gravity-mode oscillations, whereas the other frequencies may be orbital harmonics and combination terms. The ratios between the orbital frequency and the pulsation frequencies are $f_{\rm orb}$:$f_{\rm 2-4}$ $\simeq$ 2:3, which implies that the $γ$ Dor pulsations of the detached primary star may be excited by the tidal interaction of the secondary companion. The short orbital period, and the low mass ratio and $M_2$ demonstrate that KIC 6206751 is an R CMa-type star, which is most likely evolving into an EL CVn star. Of seven well-studied R CMa-type stars, our program target is the only eclipsing binary with a $γ$ Dor pulsating component.

astro-ph.SR↗

arXiv2018

State and Network Structures of Stock Markets around the Global Financial Crisis

We consider the effects of the 2008 global financial crisis on the global stock market before, during, and after the crisis. We generate complex networks from a cross-correlation matrix such as the threshold network (TN) and the minimal spanning tree (MST). In the threshold network, we assign a threshold value by using the mean and standard deviation of cross-correlation coefficients. When the threshold is equal to the mean of these coefficients, we observe a giant cluster composed of three economic zones in all three periods. We find that during the crisis, the countries in the Asian zone were weakly connected and those in the American zone were tightly linked to the countries in the European zone. At a large threshold, the three economic zones were fragmented. The European countries connected tightly, but the Asian countries bound weakly. The MST constructed from the distance matrix. In the MST, France remained a hub node in all three periods. The size of the MST shrank slightly during the crisis. We observe a scaling relation between the network distance of nodes from the central hub (France) and the geometrical distance. We observe the topological change of the financial network structure during the global financial crisis. The TN and MST are complementary roles to understand the connecting structure of financial complex networks. The TN reveals to observe the clustering effects and robustness of the cluster during the financial crisis. The MST shows the central hub and connecting node among the economic zones.

q-fin.GN↗

arXiv2018

Agent-Based Models in Social Physics

We review the agent-based models (ABM) on social physics including econophysics. The ABM consists of agent, system space, and external environment. The agent is autonomous and decides his/her behavior by interacting with the neighbors or the external environment with the rules of behavior. Agents are irrational because they have only limited information when they make decisions. They adapt using learning from past memories. Agents have various attributes and are heterogeneous. ABM is a non-equilibrium complex system that exhibits various emergence phenomena. The social complexity ABM describes human behavioral characteristics. In ABMs of econophysics, we introduce the Sugarscape model and the artificial market models. We review minority games and majority games in ABMs of game theory. Social flow ABM introduces crowding, evacuation, traffic congestion, and pedestrian dynamics. We also review ABM for opinion dynamics and voter model. We discuss features and advantages and disadvantages of Netlogo, Repast, Swarm, and Mason, which are representative platforms for implementing ABM.

physics.soc-ph↗