Theory
Observations
Using objective-prism plates, Lodén (1987, 1988, 1993) has investigated the possible population of open cluster remnants in our Galaxy under the assumption that the stars in these clusters should have similar luminosity andSimulations
Regarding numerical simulations, for systems with some 25 to 250 stars, von Hoerner (1960, 1963), Aarseth (1968) and van Albada (1968) suggested that the final outcome of the evolution of an open cluster is one or more tightly bound binaries (or even a hierarchical triple system). Van Albada pointed out several observational candidates (σ Ori, ADS 12696, ρ Oph, 1 Cas, 8 Lac and 67 Oph) as being OCRs and Wielen (1975) indicated another one, the Ursa Major moving group (Collinder 285).References
* Aarseth, S. J.; 1968, Bull. Astron. Ser., 3, 3, 105 * van Albada, T. S.; 1968, Bull. Astron. Inst. Neth., 19, 479 * Ambartsumian, V. A.; 1938, Ann. Len. State Univ., # 22, 4, 19 (English translation in: Dynamics of Star Clusters, eds. J. Goodman, P. Hut, (Dordrecht: Reidel) p. 521) * Gatewood, G.; De Jonge, J. K.; Castelaz, M.; et al., 1988, ApJ, 332, 917 * von Hoerner, S.; 1960, Z. Astrophys., 50, 184 * von Hoerner, S.; 1963, Z. Astrophys., 57, 47 * Lodén, L. O.; 1987, Ir. Astron. J., 18, 95 * Lodén, L. O.; 1988, A&SS, 142, 177 * Lodén, L. O.; 1993, A&SS, 199, 165 * Spitzer, L.; 1940, MNRAS, 100, 397 * Stefanik, R. P.; Caruso, J. R.; Torres, G.; Jha, S.; Latham, D. W.; 1997, Baltic Astronomy, 6, 137 * Upgren, A. R.; Rubin V. C.; 1965, PASP, 77, 355 * Wielen, R.; 1975, in: Dynamics of Stellar Systems, ed. A. Hayli, (Dordrecht: Reidel) p. 97 ;Further reading * Bica, E.; Santiago, B. X.; Dutra, C. M.; Dottori, H.; de Oliveira, M. R.; Pavani D., 2001, A&A, 366, 827-83