Evolution of star clusters on eccentric orbits: semi-analytical approach. (arXiv:1904.05896v1 [astro-ph.GA])

Evolution of star clusters on eccentric orbits: semi-analytical approach. (arXiv:1904.05896v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ebrahimi_H/0/1/0/all/0/1">Hamid Ebrahimi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haghi_H/0/1/0/all/0/1">Hosein Haghi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Khalaj_P/0/1/0/all/0/1">Pouria Khalaj</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zonoozi_A/0/1/0/all/0/1">Akram Hasani Zonoozi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Safaei_G/0/1/0/all/0/1">Ghasem Safaei</a>

We study the dynamical evolution of star clusters on eccentric orbits using a
semi-analytical approach. In particular we adapt and extend the equations of
EMACSS code, introduced by Gieles et al. (2014), to work with eccentric orbits.
We follow the evolution of star clusters in terms of mass, half-mass radius,
core radius, Jacobi radius and the total energy over their dissolution time.
Moreover, we compare the results of our semi-analytical models against $N$-body
computations of clusters with various initial half-mass radius, number of stars
and orbital eccentricity to cover both tidally filling and under-filling
systems. The evolution profiles of clusters obtained by our semi-analytical
approach closely follow those of $N$-body simulations in different evolutionary
phases of star clusters, from pre-collapse to post-collapse. Given that the
average runtime of our semi-analytical models is significantly less than that
of $N$-body models, our approach makes it feasible to study the evolution of
large samples of globular clusters on eccentric orbits.

We study the dynamical evolution of star clusters on eccentric orbits using a
semi-analytical approach. In particular we adapt and extend the equations of
EMACSS code, introduced by Gieles et al. (2014), to work with eccentric orbits.
We follow the evolution of star clusters in terms of mass, half-mass radius,
core radius, Jacobi radius and the total energy over their dissolution time.
Moreover, we compare the results of our semi-analytical models against $N$-body
computations of clusters with various initial half-mass radius, number of stars
and orbital eccentricity to cover both tidally filling and under-filling
systems. The evolution profiles of clusters obtained by our semi-analytical
approach closely follow those of $N$-body simulations in different evolutionary
phases of star clusters, from pre-collapse to post-collapse. Given that the
average runtime of our semi-analytical models is significantly less than that
of $N$-body models, our approach makes it feasible to study the evolution of
large samples of globular clusters on eccentric orbits.

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