Nuclear physics is the necessary link between astronomical observations, stellar models and galactic chemical evolution. The impressive progress in astrophysics during the last decades explaining and predicting astronomical scenarios was only possible because of the fruitful interplay between all disciplines. New insights in one field triggered new developments in the other fields. New experimental techniques are typically the response to new predictions and observations.
CEMP Stars as Probes of First-Star Nucleosynthesis, the IMF, and Galactic Assembly (Opens in a new window)
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.
MICRA, which stands for Microphysics In Computational Relativistic Astrophysics, is a biennial workshop focused on improving, discussing, and addressing the microphysics needs of relativistic simulations of astrophysical systems, core-collapse supernovae, compact object mergers, and gamma-ray bursts by bringing together nuclear and neutrino theorists and astrophysicists and computational modelers. This year marks the 5th installment and the 10th anniversary of MICRA, and the first since the revolutionary gravitational wave event GW170817.
The aim of the workshop is to bring the nuclear astrophysics community together to discuss opportunities available at the ATLAS facility, to foster new collaborations, and solicit new ideas for future advancement of the facility and experimental program. The ATLAS facility has undergone an expansion in its capabilities to produce and study isotopes of astrophysical interest, both through facility enhancements (CARIBU, RAISOR, the soon-to-be N=126 factory, etc.) and experimental devices/techniques (MUSIC, HELIOS, ion trapping, GRETINA, GAMMASPHERE, etc.).
Nuclear and astrophysics aspects for the rapid neutron capture process in the era of multimessenger observations (Opens in a new window)
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
The registration will be open from April 15th. For US participants, there is an opportunity to obtain travel support to ECT* workshops through the EUSTIPEN program.
An informal meeting to discuss weak interactions in hot and dense matter encountered in supernovae and neutron star mergers will be held at the Institute for Nuclear Theory June 3-6, 2019.
This is the ninth in a series of former JINA and now JINA-CEE meetings that brings together JINA-CEE participants, collaborators, and other interested researchers in nuclear physics, astronomy, and astrophysics to discuss progress and future directions related to the understanding of the origin of the elements and neutron stars.
This specialized workshop is timely as several experimental opportunities are now opening up. This workshop brings together experimentalists from several labs and the groups performing i-process nucleosynthesis calculations. We will discuss dedicated experimental and theoretical effort for improving our understanding of this process which is required for a better understanding of the origin of the heavy elements.
This is a JINA-CEE supported workshop that aims to bring together different areas of research that all involve studies of heated neutron star crusts. This includes observations of different manifestations of neutron stars, theoretical calculations and simulations, and nuclear experiments. One of the primary goals of this dedicated workshop is to have a facilitated discussion about the puzzling source of shallow crustal heating, and what observations/experiments/calculations are needed to move forward.
(i) r-process production in GR simulations of the double
neutron stars and CCSNe; the impact of neutrinos.
(ii) The assembly of double neutron stars and r-process
enrichment of the Galaxy and its satellites.
(iii) GW170827; kilonova emission from theoretical perspective.
(iv) GW170817; Modeling and observations of the associated kilonova.
(v) r-process production from the experimental nuclear physics perspective.
(vi) Observations of the r-process enhanced metal poor stars.
The purpose of the Radionuclide Astronomy in the 2020's and Beyond (RA2020) workshop is focused on determining the potential science goals in radionuclide astronomy for next-generation X-ray and gamma-ray missions. This will include identifying and prioritizing open astrophysical questions on astrophysical sources of radionuclides that can be addressed by next-generation missions.
There is a new impetus in efforts to reconcile thermonuclear burst observations and models, and also incorporate in more detail the nuclear physics inputs. At the same time, new experimental data is becoming available, that is challenging our existing understanding of burst physics.