ChETEC


Chemical Elements as Tracers of the Evolution of the Cosmos

Events

Training School - Direct nuclear reaction methods. (19-21 February, 2020. Orsay, Paris, France)
19 Feb, 2020 09:00 AM to 21 Feb, 2020 05:00 PM IPN-Orsay, Paris, France,

Various nuclear reaction methods such as transfer reactions at energies above or near the Coulomb barrier, charge-exchange reactions, ...etc, are used to analyze experimental data and determine cross-sections or reaction rates of astrophysical interest. The theoretical formalism used goes from DWBA theory (Distorded wave born approximation) to coupled channels calculations (CRC, CCBA, CDCC,...). An accurate and efficient use of the reaction codes (e.g.FRESCO) to perform the aforementioned calculations require an understanding and a practical knowledge of the underlying concepts. For this purpose, a four-day training school on direct nuclear reaction methods will be organized in the winter of 2020 at IPN-Orsay (France). The speakers will first give lectures on the principles of direct nuclear reaction methods. Then, they will show the students how to perform DWBA and coupled channel calculations using various codes, such as FRESCO, using specific practical examples.

Lithium in the Universe: to Be or not to Be? (Working Group Meeting); (18-22 November, 2019. Rome, Italy)
18 Nov, 2019 to 22 Nov, 2019 The Observatory of Rome, Monte Porzio Catone, Italy,

Among all the chemical species present in the Universe, lithium is unique for being the protagonist in several astrophysical contexts, spanning all epochs, from the Big Bang to the present day, and extending over distances from our Sun to remote regions in the Milky Way system and beyond. Lithium is currently at the centre of two highly debated mysteries that catch the attention of astrophysicists. The expected primordial value of 7Li is a factor of 3 higher than measured in warm halo dwarf stars. This discrepancy is normally referred to as the cosmological lithium problem. Since the present lithium abundance as measured in meteorites or in young stars is A(Li)=3.3, a Galactic source is required. The identification of such sources is referred to as the Galactic lithium problem.

CEMP Stars as Probes of First-Star Nucleosynthesis, the IMF, and Galactic Assembly (Working Group Meeting). (9-13 September, Geneve, Switzerland)
09 Sep, 2019 to 13 Sep, 2019 Geneva University, 30 quai Ernest Ansermet in Auditorium A100 Sciences II,

The beginning of the stellar era in the Universe is a singularly fascinating phase in the history of the Cosmos. The baryonic material filling the Universe at that time, having a composition inherited from Big Bang nucleosynthesis, has its physical characteristics modified by the very first stars. Indeed, the first stars will change the degree of ionized material in their vicinity, and, through their winds and/or supernova explosion, will inject energy, momentum, and newly-synthesized elements. Some pockets of gas, enriched by the first stars, will in turn form new stars, whose initial composition is inherited from the first nucleosynthetic events. These low-mass stars can live sufficiently long to be observed today in halo of the Galaxy, providing the opportunity to obtain information about the very high redshift Universe by the study of nearby stars. How did these processes happen? How were these processes different from similar ones occurring in the present Universe? What can they teach us about the infancy of the Universe during the reionization era? These are the questions that will be discussed during this workshop, questions that are particularly topical at a time when new facilities, such as SKA, JWST, and the next generation of extremely large telescopes have as one of their prime objectives to probe this very period. At present, observational constraints on these first stars are scarce and/or indirect. Important constraints come from observations of the elemental abundances of very, extremely, and ultra iron-poor stars that likely formed from the ejecta of the first stellar generations. Of course the full story can be complex, as some elements might be formed by more than one source, and others may be somewhat altered by in-situ processes that occurred in the star that is observed today. Nevertheless, through the accumulation of observational data, progress made in numerical simulations, and in our deeper understanding of the physical processes involved, a much more complete and detailed story can be told.

Microphysics in Computational Relativistic Astrophysics. (12-16 August, 2019. Jena, Germany)
12 Aug, 2019 09:00 AM to 16 Aug, 2019 05:00 PM Theoretisch-Physikalisches Institut at the University of Jena. JENA, GERMANY,

MICRA is a workshop (and emphatically not a conference) that heavily focuses the microphysics needs of computational simulations of astrophysical systems, neutrinos, nucleosynthesis, and nuclear density equations of state. The intention is to bring together active nuclear and neutrino theorists and astrophysicists with computational modelers to achieve improvements in the modeling of relativistic systems: stellar collapse, core-collapse supernovae (CCSNe), binary mergers, and gamma-ray bursts. Based on previous MICRAs, we envision ~40 participants from across the world, since this edition of MICRA is hosted in Europe, we expect at least 50% European participation.

Nuclear and astrophysics aspects for the rapid neutron capture process in the era of multi-messenger observations. (May 1, 2019. Trento, Italy)
01 May, 2019 from 09:00 AM to 05:00 PM ECT* (European Centre for Theoretical Studies in Nuclear Physics and Related Areas). Trento, Italy,

The rapid-neutron capture process (r-process) is responsible for producing around half of all nuclides heavier than iron. One site for the r-process was recently confirmed: the advanced LIGO and Virgo detectors observed two neutron stars merging and immediate follow-up observations were fully compatible with a kilonova, a thermal “afterglow” powered by radioactive decay of newly synthesized r-process material. Moreover, the observations indicated that neutron-star mergers produce a blue lanthanide-free signal followed by a red lanthanide-rich component, contrary to expectations. Although neutron-star mergers are now known to be r-process element factories, this might not be the only r-process site, and a comprehensive understanding and description of the r-process is still lacking. This workshop will bring together theorists and experimentalists to address the many aspects of nuclear physics and astrophysics that must be considered and properly understood in order to model the r-process.

Electron-Capture-Initiated Stellar Collapse. (20-24 May 2019, Leiden, Netherlands)
20 May, 2019 09:00 AM to 24 May, 2019 05:00 PM Lorentz center, Leiden, Netherlands,

One of the primary goals of stellar astrophysics is to connect the initial properties of stars to the remnants they leave behind. The evolution of the subset of stellar systems that experience a collapse initiated by electron-capture reactions is rich, complex and uncertain.  In particular, this workshop aims to strengthen our theoretical understanding of the type and properties of the remnants of electron-capture supernovae and accretion-induced collapse.

ChETEC Working Group 3 Workshop 2019. (From February 27 to March 1, 2019. Vilnius, Lithuania)
27 Feb, 2019 09:40 AM to 01 Mar, 2019 01:00 PM National Center for Physical Sciences and Technology, Vilnius, Lithuania,

The main goal of the workshop is the preparation of two observing proposals aimed to investigate: (a) the origin and evolution of the r-process elements in the EMP stars; (b) the origin of multiple stellar populations (MPs) in the Galactic globular clusters (GGCs); and (c) to exchange ideas regarding the possible future observing proposals related to the study of EMP stars, as well as MPs in the GGCs. Several broader review talks will set up the stage for an in-depth discussions of the two observing proposals. Separate slots will be reserved for in-depth discussions to plan future observing proposals. The largest fraction of the workshop time will be devoted to hands-on activities for writing the two observing proposals that will be submitted during the Period 104 call for proposals at ESO (March 2019). The detailed workshop program is provided below.

ChETEC Working Group 3 Workshop 2018. (14-16 March, 2018. Vilnius, Lithuania)
14 Mar, 2018 09:30 AM to 16 Mar, 2018 05:00 PM Vilnius, Lithuania,

The aim of the meeting is to tackle the following questions: (a) the preparation of the observing proposal to investigate evolution of Eu and Ba in the EMP stars; (b) discuss and take the necessary actions for the preparation of the Nuclear Astrophysics Database (NAD); and (c) discuss and launch several science projects presented at the Keele meeting in October 2017. It is foreseen that the meeting will be heavily based on discussions and interactions. Several talks will set up the stage for an in-depth discussions, with at least 10-15 min foreseen for questions and discussion after each talk. Separate slots will be reserved for longer discussions to address various important issues in detail and, ultimately, to plan further steps and actions. The meeting program is available here: https://docs.google.com/document/d/1DKDF4RFx4qvxGv9uQXCurVGyntO27jmGLF57NZ-5NUQ/edit?usp=sharing

ChETEC Code of Conduct for meeting

Every event related to ChETEC needs to make use of the following Code of conduct. It is the same a the JINA Code of Conduct, for which we gratefully acknowledge JINA.

Main Action Workshop
09 Oct, 2017 02:00 PM to 11 Oct, 2017 05:00 PM Keele,

MC meeting + WG workshops

Knowledge Hubs workshop + period 2 MC meeting
27 Jun, 2018 from 12:30 PM to 07:00 PM National Institute for Nuclear Physics - Gran Sasso National Laboratory,

During the workshop, we will review the "knowledge hubs" that we have assembled and discuss how we can improve them further. After the workshop, we will have our period(year) 2 MC meeting.

Zagreb Nucleosynthesis software pipeline training school
31 Aug, 2020 to 02 Sep, 2020 Virtual event (initially planned in Zagreb),

The ChETEC COST Action (CA16117), the IReNA NSF network of networks, and the NuGrid collaboration are organising a 3-day training school event on the topic of nuclear reaction rates, stellar nucleosynthesis, observations and implications for galactic chemical evolution.

Period 4 main event
03 Sep, 2020 to 04 Sep, 2020 Virtual event (initially planned in Split),

The ChETEC COST Action started in 2017 and is now in its fourth year/period. In this meeting, we will cover all the aspects of our Action and review all the achievements of the Action during the first three periods as well as plan period 4 and the future beyond the end of the Action.