München 2019 – scientific programme

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HK: Fachverband Physik der Hadronen und Kerne

HK 51: Nuclear Astrophysics IV

HK 51.4: Talk

Thursday, March 21, 2019, 15:00–15:15, HS 18

Exploring the astrophysical conditions for the creation of the first r-process peak — •Stylianos Nikas^1,2, Andre Sieverding^1,2, Gabriel Martinez - Pinedo^1,2, and Meng Ru Wu³ — ¹Institut für Kernphysik, Technische Universität Darmstadt, 64289 Darmstadt, Germany — ²GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291 Darmstadt, Germany — ³Institute of Astronomy and Astrophysics, Academia Sinica, Taipei, Taiwan

The r-process is responsible for the production of about half of the heavy elements observed in the solar abundances. The site of the r-process was unknown until recent observations. The gravitational wave event GW170817, which was identified as a binary Neutron Star Merger (NSM), was followed by the detection of fast fading optical counterpart consistent with the predictions for a kilonova, associated with r-process nucleosynthesis. The observation of bright, fast fading UV component, established the production of heavy element in the aftermath of NSM.

The complicated atomic structure of lanthanides implies high opacity ejecta which would shift the wavelength of the observed light to the red, the blue color of the ejecta indicates relatively high Y_e and consequently low lanthanide production. We present a study of nucleosynthesis for conditions of high Y_e outflows from NSMs and investigate the effect of various nuclear properties and the astrophysical conditions under which this could be the site for the production of the elements of the r-process abundance pattern for A <100.

This work was supported by DFG through Grant No. SFB1245 and HGS-HIRe.