Other
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...6e..30g&link_type=abstract
Neutron Stars and Black Holes in Star Clusters, 26th meeting of the IAU, Joint Discussion 6, 17-18 August 2006, Prague, Czech Re
Other
Scientific paper
In dense stellar systems it is important to understand what happens when single stars or binary star systems undergo a close encounter. One possible outcome of such an encounter is a collision followed by the merging of two or more stars. This is thought to be a formation channel for the so-called Blue Straggler stars seen in star clusters. One part of understanding stellar mergers is understanding the merging process itself, which is a hydrodynamic problem. Another part of the problem is understanding the subsequent evolution of the merger remnant, which is a stellar evolution problem. This makes it necessary to convert the hydrodynamic output to stellar evolution input, which has previously been done by Sills and Lombardi. We have created a stellar evolution code, based on the Eggleton evolution code, that can import the outcome of a hydrodynamical calculation of the merger and create a proper starting model for studying the subsequent evolution, in principle without user intervention. We have used this code to study the differences with a simplified prescription for the evolution track, lifetime and abundances for Blue Stragglers in an N-body cluster simulation by Hurley. In the future, we will use the code to compute the evolution of merger products that are the result of collisions between massive stars, which have not been studied in as great detail as the evolution of collision between low mass stars. We also plan to create a good interface between the evolution code and a hydrodynamic code that makes it easy to use the code directly in N-body simulations.
Glebbeek Evert
Pols Onno R.
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