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NuGrid Collaboration

The Nucleosynthesis Grid (NuGrid) collaboration, formed in fall 2007, develops and maintains tools for large scale post-processing nucleosynthesis simulations with up-to-date and flexible nuclear physics input, and apply these to complete sets of quiescent and explosive nuclear production environments.

Science goal

Our science goal is to provide complete sets of stellar evolution sequences for low-mass and massive stars with compatible input physics, including explosion simulations, and calculate the complete nucleosynthesis with the same post-processing code. In this way we will obtain a high degree of internal consistency. We plan to generate yield sets covering the entire mass and metallicity space, in collaboration with teams working in galactic chemical evolution and near-field cosmology.

Approach

The NuGrid approach is characterized by a commitment to forward modeling based on our physics understanding of the involved processes, verification and validation, and uncertainty quantification, including the important aspect of nuclear physics input.

NuGrid Data Release

NuGrid data Set 1 consists of 2 metallicities, Z=0.01 (set 1.1) and Z=0.02 (set 1.2) and is published in Pignatari et al. (2016). An extension of Set1 (Set1ext) adds three lower metallicites, as well as additional masses at all metallicities and MESA based massive star models for Z=0.01 and 0.02 (Ritter et al. 2017). Please go to the Yields page in the Yields folder, in the Data and software item on the left menu.

Research Areas

In addition to the primary goals the collaboration facilitates projects (in varying degrees of completion) in the following research areas (in no particular order). If you like to get in touch with NuGrid members participating in any of these projects, please get in touch with the present PI (see below).
  • Stellar evolution and nucleosynthesis
    • Massive stars
    • AGB and SAGB stars
  • Supernova explosions, explosive nucleosynthesis, core collapse and Type Ia
  • Galactic chemical evolution
  • Nucleosynthesis in compact objects (e.g., nova, RCB stars, X-ray bursts, neutron-star mergers)
  • Nuclear physics impact on stellar physics and nucleosynthesis
  • Nucleosynthesis processes (e.g., r process, rp process, i process, s process, p process)

Results

A summary of active projects and their participants can be found in the Projects folder. A list of acomplished projects can be found in the Publications folder.

Members

NuGrid is an open, flexible collaboration involving researchers from institutions from UK, USA, Canada, Italy, Switzerland, Germany and Australia. The collaboration is guided by the NuGrid Manifesto which defines the collaboration rules.

Active members

  • Keele University, UK: R. Hirschi (also Kavli IPMU (WPI), Japan), N. Nishimurap, Umberto Battinop, J. W. den Hartoghg, C. Georgyp*, A. Kozyrevap*, M. Bennettg*
  • University of Victoria, Canada: F. Herwig, Pavel Denisenkov, Christian Ritterg, Ondrea Clarksong, Austin Davisg, Laurent Dardaletg*, William Hillaryu*, Debra Richmanu*, Daniel Contiu*, Nicholas Bruceu*
  • Los Alamos National Laboratory, USA: C. L. Fryer, Aaron Couture, Wes Even, Oleg Korobkinp, A. Hungerford, Samuel Jonesp, S. Andrewsu, S. Diehl*p, G. Rockefeller*
  • Observatory of Torino, INAF, Italy: Claudia Travaglio, Sara Bisterzop
  • Arizona State University, USA: F. X. Timmes, Ilka Petermannp
  • Universtaet Frankfurt, GSI, Germany: Rene Reifarth, Kathrin Göbelp, Deniz Kurtulgilg, Christoph Köppcheng
  • TRIUMF, Canada: Chris Ruiz, Barry Davids
  • Monash University, Australia: Alexander Heger (also SJTU, Shanghai, China; UMN, Minnesota, USA), Athira Menong, James Grimmettg
  • University of Chicago, Argonnem, USA: Jim Truran, Claudio Ugaldep*
  • Michigan State University, USA: Hendrik Schatz
  • University of York, UK: Alison Laird,  Joscelyn Rileyg, Nic Hubbardg,Josh Duncanu, Chloe McElvaneyg, Ben Shawu*
  • Oak Ridge National Laboratory/University of Tennessee, USA: Michael Bertolli
  • University of Alabama, USA: Dean Townsley, Broxton Milesg
  • SUNY Stony Brook, USA: Alan Calder
  • E.A. Milne Centre for Astrophysics, University of Hull, UK: M. Pignatari, James Keegansg, Tom Lawsong, Callum Silku, Katherine Hallu, Jasmine Staintonu, Samual Lloydu, Emilio Cuanduu, Jacob Tomassiu, Ashley Tattersallu*
  • TU Munich, Germany: Shawn Bishop
  • San Diego State University, USA: Calvin Johnson
  • University of Sevilla, Institut de Fisica Corpuscolar of Valencia, Spain: Cesar Domingo Pardo, Pablo Gramage Iglesiasg, Carlos Guerrero, Jorge Lerendegui Marcg
  • UPC-Barcelona, Spain: Adria Casanovas Hosteg
  • Lawrence Livermore National Laboratory, USA: Reto Trappitschp
  • TU Darmstadt, Germany: Heiko Möllerg
  • University of Edinburgh, UK: Claudia Lederer-Woods, Ashley Tattersallg
  • Konkoly Observatory, Hungary: Benoit Côtép;
ggraduate student, uundergraduate student, ppost-doc, *project finished

Past members

  • University of Victoria, Canada: Adam Paulu, Luke Siemensu
  • E.A. Milne Centre for Astrophysics, University of Hull, UK: Jacob Brazieru
  • Basel University, Switzerland: Isabelle van Rijsu*
  • Universtaet Frankfurt, GSI, Germany: Thien Tam Ngyuenu, Paula Hillmannu, Alexander Koloczekg, Benedikt Thomasg, Tanja Heftrichp,Tanja Kauschu, Rene Schachu
  • Arizona State University, USA: Eric Deleeuwg, P. A. Young
  • Michigan State University, USA: Ulrike Hager, Richard Cyburt
  • ANU, Australia: Aaron Dotterp
  • Louisiana State Universtiy USA: Geoff Clayton, Kundam Kadamg, Ischelle Martinu
  • Notre Dame, USA: M. Beardp, Kiana Setoodehniap, G. Magkotsiosg

Collaboration PIs

The collaboration PI and Co-PIs are rotating roles that are reviewed/renewed each year. Currently, the PI of the NuGrid collaboration is Marco Pignatari (mpignatari@gmail.com), who is supported by four Co-PIs:

Points of contacts

  • Projects coordinator: Marco Pignatari
  • Membership administrator: Jacqueline den Hartogh

Codes and Collaboration Facilities

At the core of the NuGrid work is the developement, verification and validation of a post-processing nucleosynthesis code (PPN) and a variety of collaboration tools.
  • Latest nuclear physics compilations for all stellar quiescent and explosive nucleosynthesis including NSE, sandbox interface to easily test user generated rates, dynamic master network generation
  • Multi-zone with mixing for complete 1D stellar evolution sequence post-processing
  • Multi-trajectory capability for post-processing of hydrodynamic trajectories
  • Dynamic network at the cell level to automatically generate the network size needed for given thermodynamic environment
  • Multi-zone and trajectory ppn are MPI parallel
  • Custom USEEPP (se) library built on hdf5 for IO data management, including C, Fortran, python and idl interfaces
  • User code (svn’d, wiki/plone’d)
  • Data served through VOspace at CADC, interactive web exploration
  • NuGridPy python tools to analyze NuGrid data
  • NuGrid Python Chemical Evolution Environment (NuPyCEE)
The code base is now implemented and has passed verification tests for most nucleosynthesis.

Participation and Staying Connected

If you find the NuGrid project interesting please contact any of the members. We have annual collaboration meetings where we discuss the future directions, including how to make our tools available to a wider community. If you would like to receive occasional news and announcement about data releases, available NuGrid tools and new NuGrid publications, please consider signing up to the public nugrid mailing list.

Acknowlegements

NuGrid acknowledges support from NSF grants PHY 02-16783 and PHY 08-22648 (Joint Institute for Nuclear Astrophysics, JINA), NSF grant PHY-1430152 (JINA Center for the Evolution of the Elements) , EU MIRG-CT-2006-046520 and STFC (through the University of Hull’s Consolidated Grant ST/R000840/1). The continued work on codes and in disseminating data is made possible through funding from STFC (RH, UK), an NSERC Discovery grant (FH, Canada) and support from SNF (MP, Switzerland). NuGrid computations are performed at the Arizona State University's Fulton High-performance Computing Center (USA), the high-performance computer KHAOS at EPSAM Institute at Keele University (UK) as well as CFI (Canada) funded computing resources at the Department of Physics and Astronomy at the University of Victoria and through Computing Time Resource Allocation through the Compute Canada WestGrid consortium. We also acknowledge support by the STFC DiRAC High Performance Computing Facilities, and ongoing resource allocations on the University of Hulls High Performance Computing Facility viper. The collaboration uses services of the Canadian Advanced Network for Astronomy Research (CANFAR) which in turn is supported by CANARIE, Compute Canada, University of Victoria, the National Research Council of Canada, and the Canadian Space Agency. RH acknowledges support from the World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan and funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013) / ERC Grant Agreement n. 306901.

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