Destruction of open star clusters and the radius-mass relationship

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Abstract

The processes of formation and six mechanisms of disintegration of open star clusters (OSCs) are considered. Analytical estimates of the rates of OSC disintegration are made for the following mechanisms: loss of the initial gas component of OSCs, mass loss due to supernovae explosions and planetary nebula formation, pair interactions of OSC stars, acceleration of stars by binary systems of OSCs, interaction of OSC stars with stars of the Galactic disk, collisions of OSCs with giant molecular clouds (GMCs) at the front of a spiral wave. The destruction of OSCs is accompanied by the formation of a stellar stream. An analysis of the radius-mass ratio of the OSC core (RM) allowed us to conclude that it probably does not reflect the disintegration mechanism and is a product of observational selection effects. The evolution of an individual OSC in the R-M plane is determined by the initial density and external conditions.

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About the authors

A. V. Tutukov

Institute of Astronomy, Russian Academy of Sciences

Email: svvs@ya.ru
Russian Federation, Moscow

S. V. Vereshchagin

Institute of Astronomy, Russian Academy of Sciences

Author for correspondence.
Email: svvs@ya.ru
Russian Federation, Moscow

N. V. Chupina

Institute of Astronomy, Russian Academy of Sciences

Email: svvs@ya.ru
Russian Federation, Moscow

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Supplementary files

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2. Fig. 1. The structure of an open star cluster. The core and corona of the cluster are shown schematically. The stellar stream or tidal trail [5759], consisting of stars that have left the cluster, is shown by the dashed line. The stream length can reach ~1000 pc.

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3. Fig. 2. Distribution of clusters (closer than 1 kpc) from the catalog [22] by distance from the Sun (d, pc) and by logarithm of age (log t, years).

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4. Fig. 3. The logarithm of the mass - logarithm of the size relationship for the clusters in the catalog [22] located within 1 kpc of the Sun. The straight line is described by the formula log mt = 2.55(±0.063) +1.83(±0.108)log Size, where log mt is the tidal mass of the cluster in solar masses, the logarithm of the cluster size in parsecs logSize = log(d r0/57.3), where r0 is the angular size of the cluster core in degrees (Fig. 1).

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5. Fig. 4. a) The log mass - log size relationship for clusters with age log t< 8.0. The straight line is described by the formula log mt = 2.64 (±0.105) +2.05 (±0.178) log Size. b) The log mass - log size relationship for clusters with age 8.08.8. The straight line is described by the formula log mt = 2.39(±0.147)+1.52(±0.268)·log Size.

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6. Fig. 5. The relation "logarithm of tidal mass to logarithm of age" of the clusters of the catalog [22]. The color scale shows the color of the point depending on Rg (distance from the Galactic Center, CG). Among the clusters far from the CG, old clusters are observed that have survived and have a high concentration of stars toward the center of the cluster, therefore, they are better identified at distances far from the CG, against the background of a smaller number of field stars.

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