What are the astrophysical sites for the r-process and the production of heavy elements?

By Friedrich-Karl Thielemann, A. Arcones, R. Käppeli, Mathias Liebendörfer, T. Rauscher, C. Winteler, C. Fröhlich, I. Dillmann, Tobias Fischer, G. Mart'inez-Pinedo and 5 more. 2011

223 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/e1a9ba9c07b757177690b53c4085a3e9f0a15b8c

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Citations in the corpus

MAGNETOROTATIONALLY DRIVEN SUPERNOVAE AS THE ORIGIN OF EARLY GALAXY r-PROCESS ELEMENTS? (2012, methodology): “The nucleosynthesis calculations are performed with a new extended reaction network (Winteler 2011) which represents an advanced (numerically and physically) update of the BasNet network (see, e.g., Thielemann et al. (2011)).”
THE r-PROCESS NUCLEOSYNTHESIS IN THE VARIOUS JET-LIKE EXPLOSIONS OF MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE (2015, background): “…which provide suitable neutron-rich conditions, are still undetermined, although a large amount of effort by nuclear physicists, astrophysicists, and astronomers has been devoted since the dawn of modern science (for the most recent status, see, Arnould et al. 2007; Thielemann et al. 2011).”
The impact of individual nuclear properties on $r$-process nucleosynthesis (2015, background): “The site or sites of the r process still evade definitive determination [9, 10, 11].”
Neutrino-driven winds from neutron star merger remnants (2014, methodology): “For the nucleosynthesis calculations we employ the WINNET nuclear reaction network (Winteler 2012; Winteler et al. 2012), which represents an update of BASNET network code (Thielemann et al. 2011).”
Production of the entire range of r-process nuclides by black hole accretion disc outflows from neutron star mergers (2016, methodology): “The astrophysical site of this process has been under debate for more than 50 yrs (see, e.g., Qian & Wasserburg 2007, Arnould et al. 2007, Sneden et al. 2008, Thielemann et al. 2011 for reviews).”
Impact of ejecta morphology and composition on the electromagnetic signatures of neutron star mergers (2017, methodology): “We compute the compositional evolution within the ejecta with the network code WinNET (Winteler 2012; Winteler et al. 2012) that is derived from the BasNet network (Thielemann et al. 2011).”
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. IV. Detection of Near-infrared Signatures of r-process Nucleosynthesis with Gemini-South (2017, background): “…of the large neutron fluxes necessary for the r-process to occur, but most modern work has found that the conditions in numerical simulations are inadequate for the production of the heaviest r-process material in the necessary quantities (e.g., Qian & Woosley 1996; Thielemann et al. 2011).”
The Emergence of a Lanthanide-rich Kilonova Following the Merger of Two Neutron Stars (2017, methodology): “The r-process nucleosynthesis and radioactive heating are computed using the nuclear network code WinNet (Thielemann et al. 2011; Korobkin et al. 2012; Winteler et al. 2012) with a reaction rates compilation for the finite range droplet model (FRDM; Möller et al. 1995; Rauscher & Thielemann 2000).”
The long-term evolution of neutron star merger remnants – I. The impact of r-process nucleosynthesis (2013, methodology): “For the involved nucleosynthesis calculations we make use of the nuclear reaction network of Winteler (Winteler 2012; Winteler et al. 2012) which represents an update of the BasNet network (Thielemann et al. 2011).”
On the astrophysical robustness of the neutron star merger r-process (2012, methodology): “Our nucleosynthesis calculations are performed with a large reaction network (Winteler 2012; Winteler et al. 2012) that is based on the BasNet network (Thielemann et al. 2011).”
The long-term evolution of neutron star merger remnants { II. Radioactively powered transients (2013, methodology): “All the nucleosynthesis results that we are quoting here and in Paper I have been obtained with the nuclear reaction network of Winteler (Winteler 2012; Winteler et al. 2012) which is an update of the BasNet network (Thielemann et al. 2011).”