The Nucleosynthesis Grid (NuGrid) project develops and maintains tools for large scale post-processing nucleosynthesis simulations, and apply these to complete sets of quiescent and explosive nuclear production environments.
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 etal. ApJS 225:24, 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 etal. in prep). Please go to the Yields page in the Yields Folder, in the Data and software item on the left menu.
The NuGrid collaboration works actively since fall 2007 and has created a framework for large-scale nucleosynthesis simulations with up-to-date and flexible nuclear physics input.
Primary Science GoalThe initial science goal is to provide a complete set (Set 1) of stellar evolution sequences for low-mass and massive stars with compatible input physics, including simple synthetic explosion simulations for metallicity Z=0.01 and 0.02, and calculate the complete nucleosynthesis with the same post-processing code. In this way we will obtain a high degree of internal consistency. Eventually we plan to generate yield sets covering the entire mass and metallicity space, in collaboration with teams working in galaxy chemical evolution and near-field cosmology.
NuGrid mailing listsPlease sign up to the NuGrid mailing list (email@example.com) to get news and annoucmements about data releases, available NuGrid tools and new NuGrid publications. Sign up at https://lists.uvic.ca/mailman/listinfo/nugrid
Research AreasIn 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 SN type II and 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)
ApproachThe 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 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.
- 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, Benoit Cotep, Christian Ritterg, Ondrea Clarksong, Adam Paulu, Austin Davisg,Luke Siemensu, Laurent Dardaletg*, Athira Menong*, William Hillaryu*, Debra Richmanu*, Daniel Contiu*, Nicholas Bruceu*
- Basel University, Switzerland: Isabelle van Rijsu
- Los Alamos National Laboratory, NM, USA: C. L. Fryer, Aaron Couture, Wes Even, Oleg Korobkinp, A. Hungerford, S. Andrews, S. Diehl*p, G. Rockefeller*
- Observatory of Torino, INAF: Claudia Travaglio, Sara Bisterzop
- Arizona State University: F. X. Timmes, Ilka Petermannp, P. A. Young*
- Universtaet Frankfurt/GSI, Germany: Rene Reifarth, Kathrin Göbelp, Deniz Kurtulgilg, Thien Tam Ngyuenu, Paula Hillmannu, Tanja Kauschu, Alexander Koloczekg*, Benedikt Thomasg*, Tanja Heftrichp*, Rene Schachu*
- TRIUMF, Canada: Chris Ruiz, Barry Davids
- Monash University, Melbourne, Australia: Alexander Heger (also SJTU, Shanghai, China; UMN, Minnesota, USA), Athira Menong
- U Chicago/Argonnem USA: Jim Truran, Claudio Ugaldep*
- Michigan State University, USA: Hendrik Schatz, Ulrike Hager, Benoit Cotep, Eric Deleeuwg, Richard Cyburt*
- University of York, UK: Alison Laird, Joscelyn Rileyg, James Keegansg, Nic Hubbardg,Josh Duncanu, Ben Shawu*
- Oak Ridge National Laboratory/University of Tennessee, USA: Michael Bertolli
- The University of Alabama, USA: Dean Townsley
- SUNY Stony Brook, USA: Alan Calder
- E.A. Milne Centre for Astrophysics, University of Hull, United Kingdom: M. Pignatari (firstname.lastname@example.org), James Keegansg, Tom Lawsonu, Jacob Brazieru, Callum Silku, Ashley Tattersallu
- TU Munich, Germany: Shawn Bishop
- Heidelberg Institute for Theoretical Studies: Samuel Jonesp
- San Diego State University: Calvin Johnson
- Institut de fisica corpuscolar of Valencia: Cesar Domingo Pardo, Pablo Gramage Iglesiasg
- University of Sevilla: Carlos Guerrero, Jorge Lerendegui Marcg
- UPC-Barcelona: Adria Casanovas Hosteg
- Lawrence Livermore National Laboratory: Reto Trappitschp
ggraduate student, uundergraduate student, ppost-doc, *project finished
- ANU, Australia: Aaron Dotterp*
- Louisiana State Universtiy USA: Geoff Clayton*, Kundam Kadamg*, Ischelle Martinu*
- Notre Dame, USA: M. Beardp*, Kiana Setoodehniap*, G. Magkotsiosg*
The collaboration PI and Co-PIs are rotating roles that are reviewed/renewed each year. Currently, the PI of the NuGrid collaboration is Raphael Hirschi (r.hirschi AT keele.ac.uk), who is supported by four Co-PIs:
- Marco Pignatari (mpignatari AT gmail.com)
- Chris Fryer (fryer AT lanl.gov)
- Alison Laird (alison.laird AT york.ac.uk)
- Samuel Jones (Samuel.Jones AT h-its.org).
Points of contacts
Projects coordinator: Raphael Hirschi
Collaboration tools: 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
ResultsA summary of active projects and their participants is given in the Projects folder.
Please see the Publications link in the menu to the left.
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 mails with news about our work, please consider signing up to the public nugrid mailing list.
NuGrid acknowledges support from NSF grants PHY 02-16783 and PHY 09-22648 (Joint Institute for Nuclear Astrophysics, JINA), NSF grant PHY-1430152 (JINA Center for the Evolution of the Elements) and EU MIRG-CT-2006-046520. 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.