Evolution of Intermediate Mass Stellar Clusters

• Autorzy: Kowalski B. , Wiśniowski T. , Rickman H. , Wajer P.

Identyfikatory

DOI

10.32023/0001-5237/75.2.3

• Języki publikacji: EN

Abstrakty

EN

We present N-body simulations of open clusters covering a time span starting from birth and ending after 200 Myr. These clusters initially contain 5000 stars and are set up with both 3D and fractal geometries. The structural parameters are intentionally chosen so as to allow lifetimes exceeding 100 Myr. The results are analyzed with regard to bulk properties such as mass, size, number of stars, virial ratio and binary fraction, and the internal structure as evidenced by the radial profiles of mass density and stellar number density. Thus, we are able to characterize the progress of evolutionary features like mass segregation, virialization and two-body relaxation. We find that mass segregation proceeds more quickly in clusters without primordial mass segregation, likely because these allow for closer contact between low and high mass stars as two-body relaxation sets in. By studying the long-term evolution of the virial ratio, we have found that this is on average larger than the equilibrium value and shows an oscillating behavior with a characteristic frequency, possibly caused by periodic trapping of high-velocity stars in the high density region close to the center. Using simulated surface brightness profiles, we show that our cluster models are consistent with observed core radii in young clusters. We find indications that the binary fraction decreases with time in clusters without primordial mass segregation and increases in primordially mass segregated clusters. We find evidence that binary destruction and formation are continually ongoing phenomena. Primordial binaries tend to either be destroyed within 40 Myr or to exist until 200 Myr. In fractal clusters we observe both an increased binary destruction rate and an increased binary formation rate during the early times as compared to 3D clusters. This is likely due to the stars being concentrated to filaments with super-high densities.

Słowa kluczowe

EN

stars: kinematics and dynamics; open clusters and associations: general

• Wydawca: Copernicus Foundation for Polish Astronomy
• Czasopismo: Acta Astronomica
• Rocznik: 2025
• Tom: Vol. 75, No. 2
• Strony: 127--158
• Opis fizyczny: Bibliogr. 44 poz., rys., tab., wykr.

Twórcy

autor

Kowalski B.

• Centrum Badań Kosmicznych Polskiej Akademii Nauk, Bartycka 18A, 00-716, Warszawa, Poland

autor

Wiśniowski T.

• Centrum Badań Kosmicznych Polskiej Akademii Nauk, Bartycka 18A, 00-716, Warszawa, Poland

autor

Rickman H.

• Centrum Badań Kosmicznych Polskiej Akademii Nauk, Bartycka 18A, 00-716, Warszawa, Poland
• Department of Physics and Astronomy, Uppsala University, Box 516, SE-75120, Uppsala, Sweden

autor

Wajer P.

• Centrum Badań Kosmicznych Polskiej Akademii Nauk, Bartycka 18A, 00-716, Warszawa, Poland

Bibliografia

• Aarseth, S.J. 2003, “Gravitational N-Body Simulations: Tools and Algorithms”, New York, Cambridge University Press.
• Adams, F.C. 2010, Ann. Rev. Astron. and Astrophys., 48, 47.
• Adams, J.D., Stauffer, J.R., Monet, D.G., Skrutskie, M.F., and Beichman, C.A. 2001, AJ, 121, 2053.
• Adams, J.D., Stauffer, J.R., Skrutskie, M.F., et al. 2002, AJ, 124, 1570.
• Alexander, P.E.R., and Gieles, M. 2012, MNRAS, 422, 3415.
• Arya, S., Mount, D.M., Netanyahu, N.S., Silverman, R., and Wu, A.Y. 1998, Journal of the ACM, 45, 891.
• Bentley, J.L. 1975, Communications of the Association for Computing Machinery, 18, 509
• Binney, J., and Tremaine, S. 2008, “Galactic Dynamics”, Second Edition, Princeton, Princeton Univ. Press.
• Brasser, R., Duncan, M.J., Levison, H.F., Schwamb, M.E., and Brown, M.E. 2012, Icarus, 217, 1.
• Brinkmann, N., Banerjee, S., Motwani, B., and Kroupa, P. 2017, A&A, 600, A49.
• Chandrasekhar, S. 1941, ApJ, 93, 323.
• Elmegreen, B.G. 2008, ApJ, 672, 1006.
• Elson, R., Hut, P., and Inagaki, S. 1987, Ann. Rev. Astron. and Astrophys., 25, 565.
• Heggie, D.C. 1975, MNRAS, 173, 729.
• King, I. 1962, AJ, 67, 471.
• King, I. 1980, in: “Star Clusters”, IAU Symp., p. 139.
• Kraus, A.L., and Hillenbrand, L.A. 2007, AJ, 134, 2340.
• Kroupa, P. 1995, MNRAS, 277, 1522.
• Kroupa, P. 2001, MNRAS, 322, 231.
• Kroupa, P., Aarseth, S., and Hurley, J. 2001, MNRAS, 321, 699.
• Kruijssen, J.M.D. 2012, MNRAS, 426, 3008.
• Küpper, A.H.W., Maschberger, T., Kroupa, P., and Baumgardt, H. 2011, MNRAS, 417, 2300.
• Lada, C.J., and Lada, E.A. 2003, Ann. Rev. Astron. and Astrophys., 41, 57.
• Leonard, P.J.T. 1989, AJ, 98, 217.
• Leveque, A., Giersz, M., Banerjee, S., et al. 2022, MNRAS, 514, 5739.
• Lindegren, L., Klioner, S.A., Hernández, J., et al. 2021, A&A, 649, A2.
• Lynden-Bell, D. 1967, MNRAS, 136, 101.
• Oh., S., Price-Whelan, A.M., Brewer, J.M., et al. 2018, ApJ, 854, 138.
• Pang, X., Li, Y., Yu, Z., et al. 2021, ApJ, 912, 162.
• Pang, X., Wang, Y., Tang, S.-Y., et al. 2023, AJ, 166, 110.
• Parker, R.J., Goodwin, S.P., Kroupa, P., and Kouwenhoven, M.B.N. 2009, MNRAS, 397, 1577.
• Perryman, M.A.C., Brown, A.G.A., Lebreton, Y., et al. 1998, A&A, 331, 81.
• Piskunov, A.E., Schilbach, E., Kharchenko, R.V., Röser, S., and Scholz, R.-D. 2008, A&A, 477, 165.
• Plummer, H.C. 1911, MNRAS, 71, 460.
• Portegies Zwart, S.F., McMillan, S.L.W., Hut, P., and Makino, J. 2001, in: “The influence of binaries on stellar population studies”, Dordrecht, Kluwer, ASSL.264371
• Proszkow, E.-M., and Adams, F.C. 2009, ApJS, 185, 486.
• Reipurth, B., Guimarães, M.M., Connelly, M.S., and Bally, J. 2007, AJ, 134, 2272.
• Skrutskie, M.F., Cutri, R.M., Stiening, R., et al. 2006, AJ, 131, 1163.
• Spitzer, L. 1987, “Dynamical evolution of globular clusters”, Princeton, N.J., Princeton Univ. ress.
• Wajer, P., Rickman, H., Kowalski, B., and Wiśniowski, T. 2024a, Icarus, 415, 116065.
• Wajer, P., Rickman, H., Kowalski, B., and Wiśniowski, T. 2024b, Icarus, 410, 115915.
• Wang, L., Spurzem, R., Aarseth, S.J., et al. 2015, MNRAS, 450, 4070.
• Wielen, R. 1971, A&A, 13, 309.
• Wiśniowski, T., Rickman, H., Wajer, P. 2021, Acta Astron., 71, 243