Hosted by Konkoly Observatory at the Benczúr Hotel, Budapest, Hungary from Monday, August 28 2023 through Friday, September 1, 2023. 

The 1st IReNA-Ukakuren Joint Workshop “Advancing Professional Development in Nuclear Astrophysics and Beyond” will take place on August 28th - September 1, 2023, at National Astronomical Observatory of Japan (NAOJ).

This is the first workshop promoting exchange of human resources between Ukakuren and IReNA, with a core emphasis on professional development of young scientists.

The workshop will cover a wide range of research topics in nuclear astrophysics;

We are happy to announce that "The Taking the Temperature (T3): Workshop on Statistical Nuclear Physics for Astrophysics and Applications"  which was canceled due to the Covid pandemic is rescheduled now to be held from August 14-17, 2023 on the campus of Ohio University, in Athens, Ohio, USA.

The IReNA Workshop on Weak Interactions in Nuclear Astrophysics will be held at the Facility for Rare Isotope Beams (FRIB) on the campus of Michigan State University (MSU) in East Lansing, MI USA.

The workshop’s goal is to bring together researchers in both experiment and theory and from basic and applied fields, who utilize R-matrix techniques in their research. The workshop aims to address the latest developments in R-matrix theory, its application in interpreting experimental data, and its use in data evaluation.

In the context of our annual NuGrid collaboration meeting, we are hosting a half-day event with nuclear astrophysics talks, experimental and theoretical, open to the wider community. Our goal is to showcase recent results from the NuGrid collaboration and establish further connections and collaborations with interested groups.

Sign-up Link: https://forms.gle/UwFPGTPZFNntnT4L7

The workshop on Atomic and Nuclear Quantum Effects Near Threshold will provide the opportunity to discuss quantum effects that affect the cross section of nuclear reactions in low energy accelerator studies and hot plasma environments. 

The workshop will take place at the St. Leonard's Hall of the University of Edinburgh from May 31 - June 2, 2023.

Stellar spectra encode a large amount of physical information, such as a star's mass, temperature, radius, age, distance, velocity field, and detailed elemental composition. Stellar spectroscopy is used not just to study the properties of stars, but also to learn about the history of our Milky Way galaxy, the origin of elements and cosmic nucleosynthesis, the nature of dark matter, and the properties of extrasolar planets. The most common stellar atmosphere models assume Local Thermodynamic Equilibrium (LTE).

The 2023 CeNAM Frontiers in Nuclear Astrophysics Meeting will take place at the FRIB Laboratory, on the campus of Michigan State University on May 21-26, 2023. Registration and abstract submission will open late January.

The Frontiers Summer School in Nuclear Astrophysics aims to develop the cross-field knowledge of senior undergraduate and graduate students, and young researchers in the interdisciplinary field of nuclear astrophysics, via the exploration of various astrophysical and nuclear physics topics, ranging from stellar evolution and nucleosynthesis to novel experimental approaches and theoretical advances.

We are happy to announce the continuation of the successful series of workshops related to the “intermediate” or i-process nucleosynthesis. 

The workshop will take place at the Poseidonia Beach Hotel in Limassol, Cyprus during the period May 16-19, 2023. A mini school will be organized right before the main workshop ( May 15-16, 2023) for junior scientists who would benefit from an introduction and hands-on activities on i-process nucleosynthesis. 

Hosted by Eliana Masha (HZDR, Germany)

*Please note that this seminar is at 7pm ET on Thursday, April 13th*

Hosted by Kanji Mori (Fukuoka University, Japan)

This particular meeting is a twin SDSS-V/IReNA meeting whose goal is to bring researchers from two collaborations together. IReNA stands for International Research Network for Nuclear Astrophysics (https://www.irenaweb.org) and is a US-driven network that connects international nuclear astrophysics networks.

Hosted by Erin Good (Michigan State University)

The n-process is a neutron-capture process activated in Core-Collapse Supernovae (CCSNe), when the Supernova shock is passing through the deepest He-rich layers of the massive star progenitor. The peak neutron density generated is typically larger than 1018 neutrons cm-3, and the dominant neutron source is the Ne22(alpha,n)Mg25 reaction where the Ne22 available was left in the ashes of the hydrostatic convective He shell.

The 18th Russbach School on Nuclear Astrophysics will take place in the village of Rußbach am Paß Gschütt, southeast of Salzburg, Austria. The school dates will be from March 12 (arrival and registration) to March 18 (departure) 2023.

Understanding the behavior of white dwarfs in interacting binary systems is critical to determining the rates, distributions, and chemical contributions from transients such as novae and type Ia supernovae. In this talk I will be presenting results from my recent work on novae, which combines population synthesis (binary_c) and galactic chemical evolution modeling (OMEGA+).

Understanding how the heavy elements came into being in the universe presents one of the greatest challenges in nuclear physics and astrophysics.  For some time we have known that elements beyond iron on the periodic table must have been made through neutron-induced reactions, but the environments where they are made and what they can tell us about this history of our galaxy remain a mystery.

Carbon is produced in stars mainly via the triple-alpha process where three helium nuclei fuse to form an excited state of carbon-12 known as the Hoyle state. This is a nuclear resonance (an excited form of a nucleus) that has properties that guide the rate that the triple alpha process takes place. Primarily, the key property is how often the Hoyle state is able to lose energy and end up in the ground state of carbon-12 – known as the radiative width.