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r-Process Nucleosynthesis in Neutron Star Mergers with the New Nuclear Reaction Network SkyNet

Citation

Lippuner, Jonas (2018) r-Process Nucleosynthesis in Neutron Star Mergers with the New Nuclear Reaction Network SkyNet. Dissertation (Ph.D.), California Institute of Technology. doi:10.7907/Z9V40SCS. http://resolver.caltech.edu/CaltechTHESIS:06072017-212011532

Abstract

At the Big Bang, only the lightest elements, mainly hydrogen and helium, were produced. Stars synthesize heavier elements, such as helium, carbon, and oxygen, from lighter ones through nuclear fusion. Iron-group elements are created in supernovae (both type Ia and core-collapse). It has been known for 60 years that the slow and rapid neutron capture processes (s- and r-process) are each responsible for creating about half of the elements beyond the iron group. The s-process is known to occur in asymptotic giant branch stars, but the astrophysical site of the r-process is still a mystery. Based on observations of heavy elements in old stars, it was theorized that r-process nucleosynthesis takes place in core-collapse supernovae (CCSNe). However, recent CCSN simulations indicate that the conditions required for the r-process are not obtained in CCSN. The focus has thus shifted to neutron star mergers (both binary neutron star and black hole-neutron star mergers), where the r-process easily synthesizes all the known heavy elements. Neutron star mergers are expected to be detected by the Laser Interferometer Gravitational Wave Observatory (LIGO) in the near future, which should either confirm or rule out their proposed association with radioactively powered transients called kilonovae or macronovae that are the observational signatures of r-process nucleosynthesis. To understand how the r-process operates in different astrophysical scenarios and what relative abundance patterns it produces, detailed nuclear reaction network calculations are needed that track thousands of isotopes and tens of thousands of nuclear reactions. In this thesis, I present SkyNet, a new general-purpose nuclear reaction network that can evolve an arbitrary list of nuclear species with an arbitrary set of nuclear reactions. I describe in detail the different physics that is implemented in SkyNet and I perform code tests and comparisons to other nuclear reaction networks. Then I use SkyNet to systematically investigate r-process nucleosynthesis as a function of the initial electron fraction, initial entropy, and expansion timescale of the fluid. Further, I present r-process nucleosynthesis calculations with SkyNet in the dynamical ejecta of a black hole–neutron star merger with varying levels of neutrino irradiation. Finally, I study the r-process in the outflow of a neutron star merger remnant disk as a function of the lifetime of the central hypermassive neutron star (HMNS). SkyNet is easy to use and flexible and it is publicly available as open-source software. Multiple researchers are already using SkyNet for their work, and I hope that SkyNet will be a useful tool for the broader nuclear astrophysics community.

Item Type:Thesis (Dissertation (Ph.D.))
Subject Keywords:nucleosynthesis; nuclear reaction network
Degree Grantor:California Institute of Technology
Division:Physics, Mathematics and Astronomy
Major Option:Physics
Thesis Availability:Public (worldwide access)
Research Advisor(s):
  • Ott, Christian D.
Group:TAPIR
Thesis Committee:
  • Ott, Christian D. (chair)
  • Filippone, Bradley W.
  • Kulkarni, Shrinivas R.
  • Metzger, Brian D.
  • Roberts, Luke F.
Defense Date:22 June 2017
Non-Caltech Author Email:jonas (AT) lippuner.ca
Funders:
Funding AgencyGrant Number
National Science FoundationPHY-1151197
National Science FoundationAST-1333520
National Science FoundationAST-1205732
National Science FoundationPHY-0960291
National Science FoundationPHY-1430152
Sherman Fairchild FoundationUNSPECIFIED
Record Number:CaltechTHESIS:06072017-212011532
Persistent URL:http://resolver.caltech.edu/CaltechTHESIS:06072017-212011532
DOI:10.7907/Z9V40SCS
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1706.06198arXivChapter II
https://doi.org/10.1088/0004-637X/815/2/82DOIChapter III
https://doi.org/10.1093/mnras/stw2622DOIChapter IV
http://arxiv.org/abs/1703.06216arXivChapter V
http://dx.doi.org/10.1103/PhysRevD.93.044019DOIOther work
http://dx.doi.org/10.1103/PhysRevD.93.044064DOIOther work
http://dx.doi.org/10.1093/mnras/stw1227DOIOther work
http://dx.doi.org/10.1103/PhysRevD.93.124062DOIOther work
http://dx.doi.org/10.3847/2041-8213/834/1/L2DOIOther work
http://dx.doi.org/10.1093/mnras/stx478DOIOther work
http://dx.doi.org/10.1016/j.jcp.2016.12.059DOIOther work
http://dx.doi.org/10.1088/1361-6382/aa7a77DOIOther work
https://developer.nvidia.com/ncclOtherOther work
http://jonaslippuner.com/cvCurriculum VitaeAuthor CV
http://adsabs.harvard.edu/cgi-bin/nph-abs_connect?library&libname=Papers&libid=50a08b4b01ADSPublication list
https://arxiv.org/a/lippuner_j_1.htmlarXivPublication list
http://jonaslippuner.com/skynet/SkyNet_Ye_0.010_s_010.000_tau_007.100.mp4Streaming VideoNucleosynthesis movie
https://bitbucket.org/jlippuner/skynetOtherSkyNet source code
ORCID:
AuthorORCID
Lippuner, Jonas0000-0002-5936-3485
Default Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:10312
Collection:CaltechTHESIS
Deposited By: Jonas Lippuner
Deposited On:13 Jul 2017 15:44
Last Modified:13 Jul 2017 16:03

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