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Predictions for the hydrogen-free ejecta of pulsational pair-instability supernovae

Renzo, M.; Farmer, R.; Justham, S.; Gotberg, Y.; de Mink,. S. E.; Zapartas, E.; Marchant, P.; Smith, N.


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  <identifier identifierType="DOI">10.5281/zenodo.3406357</identifier>
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    <creator>
      <creatorName>Renzo, M.</creatorName>
      <givenName>M.</givenName>
      <familyName>Renzo</familyName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="http://orcid.org/">0000-0002-6718-9472</nameIdentifier>
      <affiliation>Flatiron Institute, CCA</affiliation>
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      <creatorName>Farmer, R.</creatorName>
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      <familyName>Farmer</familyName>
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      <affiliation>University of Amsterdam, API</affiliation>
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      <creatorName>Justham, S.</creatorName>
      <givenName>S.</givenName>
      <familyName>Justham</familyName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="http://orcid.org/">0000-0001-7969-1569</nameIdentifier>
      <affiliation>Chinese accademy of Science</affiliation>
    </creator>
    <creator>
      <creatorName>Gotberg, Y.</creatorName>
      <givenName>Y.</givenName>
      <familyName>Gotberg</familyName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="http://orcid.org/">0000-0002-6960-6911</nameIdentifier>
      <affiliation>The observatories of the Carnegie institution</affiliation>
    </creator>
    <creator>
      <creatorName>de Mink,. S. E.</creatorName>
      <givenName>. S. E.</givenName>
      <familyName>de Mink</familyName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="http://orcid.org/">0000-0001-9336-2825</nameIdentifier>
      <affiliation>Harvard, CfA</affiliation>
    </creator>
    <creator>
      <creatorName>Zapartas, E.</creatorName>
      <givenName>E.</givenName>
      <familyName>Zapartas</familyName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="http://orcid.org/">0000-0002-7464-498X</nameIdentifier>
      <affiliation>Geneva Observatory</affiliation>
    </creator>
    <creator>
      <creatorName>Marchant, P.</creatorName>
      <givenName>P.</givenName>
      <familyName>Marchant</familyName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="http://orcid.org/">0000-0002-0338-8181</nameIdentifier>
      <affiliation>KU Leuven</affiliation>
    </creator>
    <creator>
      <creatorName>Smith, N.</creatorName>
      <givenName>N.</givenName>
      <familyName>Smith</familyName>
      <affiliation>Steward Observatory</affiliation>
    </creator>
  </creators>
  <titles>
    <title>Predictions for the hydrogen-free ejecta of pulsational pair-instability supernovae</title>
  </titles>
  <publisher>Zenodo</publisher>
  <publicationYear>2019</publicationYear>
  <subjects>
    <subject>Massive stars</subject>
    <subject>pulsational pair instability supernovae</subject>
    <subject>circumstellar material</subject>
    <subject>black holes</subject>
  </subjects>
  <dates>
    <date dateType="Issued">2019-09-12</date>
  </dates>
  <language>en</language>
  <resourceType resourceTypeGeneral="Text">Journal article</resourceType>
  <alternateIdentifiers>
    <alternateIdentifier alternateIdentifierType="url">https://zenodo.org/record/3406357</alternateIdentifier>
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    <relatedIdentifier relatedIdentifierType="URL" relationType="IsPartOf">https://zenodo.org/communities/astronomy-general</relatedIdentifier>
  </relatedIdentifiers>
  <rightsList>
    <rights rightsURI="https://creativecommons.org/licenses/by/4.0/legalcode">Creative Commons Attribution 4.0 International</rights>
    <rights rightsURI="info:eu-repo/semantics/openAccess">Open Access</rights>
  </rightsList>
  <descriptions>
    <description descriptionType="Abstract">&lt;p&gt;Numerical results of the simulations presented in Renzo, Farmer, et al. 2020 (https://ui.adsabs.harvard.edu/abs/2020arXiv200205077R/abstract)&lt;br&gt;
&lt;br&gt;
Models are named as MASS_ZX.tar.gz, where MASS is the initial He core mass in solar mass units, and X is the metallicity of the models. H-rich140.tar.gz contains the files for the H-rich model of Appendix B.&lt;br&gt;
&lt;br&gt;
Each tarball contains the history file, a few MESA profile saved at specific evolutionary phases (before turning on the hydro in MESA at each pulse and at the onset of core-collapse), and the file ejecta.data which contains the properties of the ejecta at the time they first become faster than the escape velocity. These can be used as input in CSM simulations. We also provide the input files to reproduce each model in the corresponding tarball, and template input files at mesastar.org.&lt;/p&gt;</description>
  </descriptions>
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