The catalogue of structural and dynamical characteristics of 103 open star clusters and the firstresults of its investigation

Данилов, В. А.; Seleznev, A. F.

doi:10.1080/10556799408232061

Cited by 34 publications

(32 citation statements)

References 19 publications

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“…Especially in segregated clusters, due to energy equipartition the brightest stars are more concentrated to the cluster centre, and do not reproduce the correct tidal radius. Nevertheless, for distant clusters we can see a distance-dependent effect only in the upper panel of Fig.6, where we compare our masses with those of Danilov and Seleznev (1994). Since the M D /M C -relations decrease with distance modulus, we suppose that our method manages biases better than the approach by Danilov and Seleznev (1994).…”

Section: Various Scales Of Cluster Massesmentioning

confidence: 76%

“…In Fig.6 we compare the different results on mass estimates. Danilov & Seleznev (1994) derived masses for 103 compact, distant (>1 kpc) clusters from star counts down to B = 16 from homogeneous wide-field observations with the 50-cm Schmidt camera of the Ural university. For each cluster, the authors estimated the average mass of a star observed in a cluster and then computed the total visible cluster mass.…”

Section: Various Scales Of Cluster Massesmentioning

confidence: 99%

“…In fact, this method could be applied with reasonable degree of safety to the nearest clusters observed with deep, wide-area surveys, and so providing secure and complete membership. Due to its simplicity the method is currently widely accepted, and possibly it is the only technique which is applied to relatively large samples of open clusters (see Danilov & Seleznev 1994, Tadross et al 2002, and Lamers et al 2005.…”

Section: Introductionmentioning

confidence: 99%

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Towards absolute scales for the radii and masses of open clusters

Пискунов

Schilbach

Kharchenko

et al. 2007

A&A

131

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Aims. In this paper we derive tidal radii and masses of open clusters in the nearest kiloparsecs around the Sun. Methods. For each cluster, the mass is estimated from tidal radii determined from a fitting of three-parametric King's profiles to the observed integrated density distribution. Different samples of members are investigated. Results.For 236 open clusters, all contained in the catalogue ASCC-2.5, we obtain core and tidal radii, as well as tidal masses. The distributions of the core and tidal radii peak at about 1.5 pc and 7 -10 pc, respectively. A typical relative error of the core radius lies between 15% and 50%, whereas, for the majority of clusters, the tidal radius was determined with a relative accuracy better than 20%. Most of the clusters have tidal masses between 50 and 1000 m⊙, and for about half of the clusters, the masses were obtained with a relative error better than 50%.

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Section: Various Scales Of Cluster Massesmentioning

confidence: 76%

Section: Various Scales Of Cluster Massesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Towards absolute scales for the radii and masses of open clusters

Пискунов

Schilbach

Kharchenko

et al. 2007

A&A

131

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“…A detailed study of stellar velocities in OCls from the list [52] may provide further data (in addition to those already obtained by Danilov and Putkov [49], which are available at http://cdsarc.u-strasbg.fr/cgi-bin/ /Vizier?-source=J/AZh/89/674) on the non-stationarity of these clusters and the instability of PSD fluctuations marked by the " * " subscript in Table 2. Such a study may use the radial variations of the stellar velocity dispersion in the cluster and the dispersions of tangential and radial velocities of the stars in the extended neighborhoods of these clusters (the increase of stellar velocity dispersion with clustercentric distance is an important kinematic indicator of OCl nonstationarity [34]).…”

Section: ) νmentioning

confidence: 93%

Correlations, spectra, and instability of phase-space density fluctuations in open-cluster models

Данилов

Putkov

2013

Astrophys. Bull.

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Abstract-The dynamical evolution of six open star cluster models is analyzed using the correlation and spectral analysis of phase-space density fluctuations. The two-time and mutual correlation functions are computed for the fluctuations of the phase-space density of cluster models. The data for two-time and two-particle correlations are used to determine the correlation time for phase-space density fluctuations ((0.1-1) τ v.r. , where τ v.r. is the violent relaxation time of the model) and the average phase velocities of the propagation of such fluctuations in cluster models. These velocities are 2-20 times smaller than the root mean square velocities of the stars in the cluster core. The power spectra and dispersion curves of phase-space density fluctuations are computed using the Fourier transform of mutual correlation functions. The results confirm the presence of known unstable phase-space density fluctuations due to homologous fluctuations of the cluster cores. The models are found to exhibit a number of new unstable phase-space density fluctuations (up to 32-41 pairs of fluctuations with different complex conjugate frequencies in each model; the e-folding time of the amplitude growth of such fluctuations is (0.4-10) τ v.r. and their phases are distributed rather uniformly). Astrophysical applications of the obtained results (irregular structure of open star clusters, formation and decay of quasi-stationary states in such clusters) are discussed. DOI: 10.1134/S199034131302003X Keywords: stars: kinematics and dynamics-Galaxy: open clusters and associations: general INTRODUCTIONRecently, Chavanis [1-3] derived theoretical estimates for the fluctuations of phase-space density (PSD) and the corresponding correlation functions for spatially uniform and nonuniform systems with long-range interactions (including self-gravitating systems). To this end, the above author used kinetic equations written with a number of simplifying assumptions. The formulas for the correlation functions derived by Chavanis [1-3] have a rather complex form making them difficult to use for analyzing dynamic processes in such systems. In our opinion, it is more productive to compute the correlation functions directly by numerically integrating the equations of motion of gravitating particles in the problems of clustering of galaxies and the evolution of the Universe (see, e.g., [4][5][6]), and also when modeling the dynamics of open star clusters (OCl) [7].In one of our previous papers [7] we computed the two-time correlation functions for r = |r|, v = |v|, and the energy ε per unit star mass, as well as twoparticle correlations of r, v, ε, stellar number density n = n(r, t) and PSD f = f (r, v, t) for open star

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“…Given that the maximum radii of open clusters do not exceed 10-15 pc [22], it is safe to suggest that the eclipsing system SZ Cam is not a member of the NGC 1502 open cluster onto whose center it projects.…”

Section: Estimates Of the Mass Of The Third Body And The Distance To mentioning

confidence: 99%

Parameters of the apparent relative orbit of the third body in the SZ Cam system

Gorda¹,

Balega

Pluzhnik

et al. 2007

Astrophys. Bull.

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The catalogue of structural and dynamical characteristics of 103 open star clusters and the firstresults of its investigation

Cited by 34 publications

References 19 publications

Towards absolute scales for the radii and masses of open clusters

Towards absolute scales for the radii and masses of open clusters

Correlations, spectra, and instability of phase-space density fluctuations in open-cluster models

Parameters of the apparent relative orbit of the third body in the SZ Cam system

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