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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.
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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.
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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. 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.
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.
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.
This workshop aims to strengthen our theoretical understanding of the type and properties of the remnants of electron-capture supernovae and accretion-induced collapse.
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.
Conference and satellite workshop (ChETEC) in Heidelberg, Germany. Abstract and details can be found on the listed web page.
A 1-day meeting discussing the technological challenge in Nuclear Astrophysics
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.
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.
MC meeting + WG workshops
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.
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.
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.