{ "id": "1509.07628", "version": "v1", "published": "2015-09-25T08:31:18.000Z", "updated": "2015-09-25T08:31:18.000Z", "title": "Nucleosynthesis in the Ejecta of Neutron Star Mergers", "authors": [ "Dirk Martin", "Albino Perego", "Almudena Arcones", "Oleg Korobkin", "Friedrich-Karl Thielemann" ], "comment": "6 pages, 4 figures, accepted for publication on PoS", "categories": [ "astro-ph.SR", "astro-ph.HE", "nucl-th" ], "abstract": "Heavy elements like gold, platinum or uranium are produced in the r-process, which needs neutron-rich and explosive environments. Neutron star mergers are a promising candidate for an r-process site. They exhibit three different channels for matter ejection fulfilling these conditions: dynamic ejecta due to tidal torques, neutrino-driven winds and evaporating matter from the accretion disk. We present a first study of the integrated nucleosynthesis for a neutrino-driven wind from a neutron star merger with a hyper-massive neutron star. Trajectories from a recent hydrodynamical simulation are divided into four different angle regions and post-processed with a reaction network. We find that the electron fraction varies around $Y_e \\approx 0.1 - 0.4$, but its distribution differs for every angle of ejection. Hence, the wind ejecta do not undergo a robust r-process, but rather possess distinct nucleosynthesis yields depending on the angle range. Compared to the dynamic ejecta, a smaller amount of neutron-rich matter gets unbound, but the production of lighter heavy elements with $A \\lesssim 130$ in the neutrino-driven wind can complement the strong r-process of the dynamic ejecta.", "revisions": [ { "version": "v1", "updated": "2015-09-25T08:31:18.000Z" } ], "analyses": { "keywords": [ "neutron star merger", "neutrino-driven wind", "dynamic ejecta", "possess distinct nucleosynthesis yields", "electron fraction varies" ], "note": { "typesetting": "TeX", "pages": 6, "language": "en", "license": "arXiv", "status": "editable", "adsabs": "2015arXiv150907628M", "inspire": 1394836 } } }