TY - JOUR
T1 - Supernova fallback
T2 - A possible site for the r-process
AU - Fryer, Christopher L.
AU - Herwig, Falk
AU - Hungerford, Aimee
AU - Timmes, Francis
N1 - Funding Information:
Cowan, Brad Meyer, Hendrik Schatz, and Jim Truran for pragmatic discussions. This work was funded in part under the auspices of the US Department of Energy and supported by its contract W-7405-ENG-36 to Los Alamos National Laboratory and by DOE SciDAC grant DE-FC02-01ER41176.
PY - 2006/8/1
Y1 - 2006/8/1
N2 - The conditions for the leading r-process site candidate, neutrino-driven winds, cannot be reproduced self-consistently in current supernova models. For that reason, we investigate an alternate model involving the mass ejected by fallback in a supernova explosion, through hydrodynamic and nucleosynthesis calculations. The nucleosynthetic products of this ejected material produce r-process elements, including those in the vicinity of the elusive third peak at mass number 195.9 Trans-iron element production beyond the second peak is made possible by a rapid (<1 ms) freezeout of α-particles that leaves behind a large nucleon (including protons!) to r-process seed ratio. This rapid phase is followed by a relatively long (≳ 15 ms) simmering phase at ∼2 × 10 K, which is the thermodynamic consequence of the hydrodynamic trajectory of the turbulent flows in the fallback outburst. During the slow phase, high-mass elements beyond the second peak are first made through rapid capture of both protons and neutrons. The flow stays close to the valley of stability during this phase. After freezeout of protons the remaining neutrons cause a shift out to short-lived isotopes, as is typical for the r-process. A low electron fraction, is not required in this model; however, the detailed final distribution is sensitive to the electron fraction. Our simulations suggest that supernova fallback is a viable alternative scenario for the r-process.
AB - The conditions for the leading r-process site candidate, neutrino-driven winds, cannot be reproduced self-consistently in current supernova models. For that reason, we investigate an alternate model involving the mass ejected by fallback in a supernova explosion, through hydrodynamic and nucleosynthesis calculations. The nucleosynthetic products of this ejected material produce r-process elements, including those in the vicinity of the elusive third peak at mass number 195.9 Trans-iron element production beyond the second peak is made possible by a rapid (<1 ms) freezeout of α-particles that leaves behind a large nucleon (including protons!) to r-process seed ratio. This rapid phase is followed by a relatively long (≳ 15 ms) simmering phase at ∼2 × 10 K, which is the thermodynamic consequence of the hydrodynamic trajectory of the turbulent flows in the fallback outburst. During the slow phase, high-mass elements beyond the second peak are first made through rapid capture of both protons and neutrons. The flow stays close to the valley of stability during this phase. After freezeout of protons the remaining neutrons cause a shift out to short-lived isotopes, as is typical for the r-process. A low electron fraction, is not required in this model; however, the detailed final distribution is sensitive to the electron fraction. Our simulations suggest that supernova fallback is a viable alternative scenario for the r-process.
KW - Nuclear reactions, nucleosynthesis, abundances
KW - Supernovae: general
UR - http://www.scopus.com/inward/record.url?scp=33748050772&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=33748050772&partnerID=8YFLogxK
U2 - 10.1086/507071
DO - 10.1086/507071
M3 - Article
AN - SCOPUS:33748050772
SN - 0004-637X
VL - 646
SP - L131-L134
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2 II
ER -