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Clusters in the solar neighbourhood: how are they destroyed?

Lamers, HJGLM and Gieles, M (2006) Clusters in the solar neighbourhood: how are they destroyed?

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Abstract

We predict the survival time of initially bound star clusters in the solar neighbourhood taking into account: (1) stellar evolution, (2) tidal stripping, (3) shocking by spiral arms and (4) encounters with giant molecular clouds. We find that the predicted dissolution time is t_dis= 1.7 (M_i/10^4 M_sun)^0.67 Gyr for clusters in the mass range of 10^2 < M_i < 10^5 M_sun, where M_i is the initial mass of the cluster.. The resulting predicted shape of the logarithmic age distribution agrees very well with the empirical one, derived from a complete sample of clusters in the solar neighbourhood within 600 pc. The required scaling factor implies a star formation rate of 400 M_sun/Myr within 600 pc from the Sun or a surface formation rate of 3.5 10^-10 M_sun/(yr pc^2) for stars in bound clusters with an initial mass in the range of 10^2 to 3 10^4 M_sun.

Item Type: Article
Authors :
NameEmailORCID
Lamers, HJGLMUNSPECIFIEDUNSPECIFIED
Gieles, Mm.gieles@surrey.ac.ukUNSPECIFIED
Date : 30 June 2006
Identification Number : https://doi.org/10.1051/0004-6361:20065567
Uncontrolled Keywords : astro-ph, astro-ph
Related URLs :
Depositing User : Symplectic Elements
Date Deposited : 17 May 2017 12:40
Last Modified : 17 May 2017 15:05
URI: http://epubs.surrey.ac.uk/id/eprint/836249

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