Numerical simulations of tidal tails for the open cluster NGC 188

Chumak, Yaroslav; Platais, I.; McLaughlin, Dean E.; Rastorguev, A. S.; Chumak, O. V.

doi:10.1111/j.1365-2966.2009.16021.x

Cited by 48 publications

(51 citation statements)

References 41 publications

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“…The study of tidal interactions in the open clusters plays an important role in understanding the initial structure and dynamic evolution of the clusters (Chumak et al 2010;Dalessandro et al 2015). The tidal radius is described as the radial distance from the cluster center where gravitational acceleration caused by the cluster is almost equal to the tidal acceleration caused due to the Galaxy (von Hoerner 1957).…”

Section: Tidal Radiusmentioning

confidence: 99%

Photometric, kinematic, and variability study in the young open cluster NGC 1960

Joshi

Maurya

John

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a comprehensive photometric analysis of a young open cluster NGC 1960 (= M36) along with the long-term variability study of this cluster. Based on the kinematic data of Gaia DR2, the membership probabilities of 3871 stars are ascertained in the cluster field among which 262 stars are found to be cluster members. Considering the kinematic and trigonometric measurements of the cluster members, we estimate a mean cluster parallax of 0.86±0.05 mas and mean proper motions of µ RA = -0.143±0.008 mas yr −1 , µ Dec = -3.395±0.008 mas yr −1 . We obtain basic parameters of the cluster such as E(B − V) = 0.24±0.02 mag, log(Age/yr)=7.44±0.02, and d = 1.17±0.06 kpc. The mass function slope in the cluster for the stars in the mass range of 0.72-7.32 M ⊙ is found to be γ = -1.26±0.19. We find that mass segregation is still taking place in the cluster which is yet to be dynamically relaxed. This work also presents first high-precision variability survey in the central 13 ′ × 13 ′ region of the cluster. The V band photometric data accumulated on 43 nights over a period of more than 3 years reveals 76 variable stars among which 72 are periodic variables. Among them, 59 are short-period (P < 1 day)and 13 are long-period (P > 1 day). The variable stars have V magnitudes ranging between 9.1 to 19.4 mag and periods between 41 minutes to 10.74 days. On the basis of their locations in the H-R diagram, periods and characteristic light curves, the 20 periodic variables belong to the cluster. We classified them as 2 δ-Scuti, 3 γ-Dor, 2 slowly pulsating B stars, 5 rotational variables, 2 non-pulsating B stars and 6 as miscellaneous variables.

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Section: Tidal Radiusmentioning

confidence: 99%

Photometric, kinematic, and variability study in the young open cluster NGC 1960

Joshi

Maurya

John

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…We estimate central densities for the open clusters using a simple Plummer model, ρ(r 0 ) = 3M Pl 4πR 3 Pl , where M Pl is the total mass and R Pl is the half-mass radius (e.g. Chumak et al 2010).…”

Section: Open Clustersmentioning

confidence: 99%

The X-ray emissivity of low-density stellar populations

Heinke

Ivanov

Koch

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The dynamical production of low-mass X-ray binaries and brighter cataclysmic variables (CVs) in dense globular clusters is well-established. We investigate how the X-ray emissivity of fainter X-ray binaries (principally CVs and coronally active binaries) varies between different environments. We compile calculations (largely from the literature) of the X-ray emissivity of old stellar populations, including open and globular clusters and several galaxies. We investigate three literature claims of unusual X-ray sources in low-density stellar populations. We show that a suggested quiescent neutron star in the open cluster NGC 6819 is a foreground M dwarf. We show that the suggested diffuse X-ray emission from an old nova shell in the globular cluster NGC 6366 is actually a background galaxy cluster. And we show that a suggested population of quiescent X-ray binaries in the Sculptor Dwarf Galaxy is mostly (perhaps entirely) background galaxies. We find that above densities of 10 4 M /pc 3 , the X-ray emissivity of globular clusters increases, due to dynamical production of X-ray emitting systems. Below this density, globular clusters have lower X-ray emissivity than the other populations, and we do not see a strong dependence of X-ray emissivity due to density effects. We find significant correlations between X-ray emissivity and binary fraction, metallicity, and density. Sampling these fits via bootstrap techniques gives less significant correlations, but confirms the effect of metallicity on low-density populations, and that of density on the full globular cluster sample.

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“…The tidal interactions are very important in understanding the initial structure as well as the dynamic evolution of the clusters (Dalessandro et al 2015;Chumak et al 2010). The tidal radius is defined as the distance from the center of a cluster where the gravitational acceleration caused by the cluster becomes equal to the tidal acceleration due to the parent Galaxy (von Hoerner 1957).…”

Section: Tidal Radiusmentioning

confidence: 99%

Photometric and kinematic study of the three intermediate age open clusters NGC 381, NGC 2360, and Berkeley 68

Maurya

Joshi

2020

Monthly Notices of the Royal Astronomical Society

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We present UBVR c I c photometric study of three intermediate age open star clusters NGC 381, NGC 2360, and Berkeley 68 (Be 68). We examine the cluster membership of stars using recently released Gaia DR2 proper motions and obtain a total of 116, 332, and 264 member stars in these three clusters. The mean reddening of E(B − V) = 0.36±0.04, 0.08±0.03, and 0.52±0.04 mag are found in the direction of these clusters where we observe an anomalous reddening towards NGC 381. We fitted the solar metallicity isochrones to determine age and distance of the clusters which are found to be log(Age) = 8.65±0.05, 8.95±0.05, and 9.25±0.05 yr with the respective distance of 957±152, 982±132, and 2554±387 pc for the clusters NGC 381, NGC 2360, and Be 68. A two-stage power law in the mass function (MF) slope is observed in the cluster NGC 381, however, we observe only a single MF slope in the clusters NGC 2360 and Be68. To study a possible spatial variation in the slope of MF we estimate slopes separately in the inner and the outer regions of these clusters and notice a steeper slope in outer region. The dynamic study of these clusters reveals deficiency of lowmass stars in their inner regions suggesting the mass segregation process in all these clusters. The relaxation times of 48.5, 78.9, and 87.6 Myr are obtained for the clusters NGC 381, NGC 2360, and Be 68, respectively which are well below to their respective ages. This suggests that all the clusters are dynamically relaxed.

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Numerical simulations of tidal tails for the open cluster NGC 188

Cited by 48 publications

References 41 publications

Photometric, kinematic, and variability study in the young open cluster NGC 1960

Photometric, kinematic, and variability study in the young open cluster NGC 1960

The X-ray emissivity of low-density stellar populations

Photometric and kinematic study of the three intermediate age open clusters NGC 381, NGC 2360, and Berkeley 68

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