Welcome

• Konrad Schmidt (Helmholtz-Zentrum Dresden-Rossendorf, Germany)

Room: virtual

Carpathian Summer School of Physics

• Livius Trache (Horia Hulubei National Institute for Physics & Nuclear Engineering, Romania)

Room: virtual Introduction of the school and invitation to the Carpathian Summer School of Physics from August 18 to 27, 2021

Nuclear physics in astrophysics studies with direct methods using small accelerators

• György Gyürky (ATOMKI, Hungary)

Room: virtual

Moderated questions

• Rosario Gianluca Pizzone (Laboratori Nazionali del Sud, Italy)

Room: virtual

Nuclear equation of state and physics of compact stars

• Adriana Raduta (Horia Hulubei National Institute for Physics & Nuclear Engineering, Romania)

Room: virtual

Moderated questions

• Olivier Sorlin (Grand Accélérateur National d'Ions Lourds, France)

Room: virtual

From nuclei to stars – a case in point

• Adriana Banu (James Madison University, United States)

Room: virtual Photoneutron reaction cross section measurements on Molybdenum-94 and Zirconium-90 relevant to the p process nucleosynthesis

Moderated questions

• Aurora Tumino (Kore University of Enna, Italy)

Room: virtual

Breakout session Room: virtual Breakout rooms are available to (1) very briefly introduce yourself, (2) talk about the lectures, (3) clarify lecture items, and (4) phrase questions for the round table discussion. Afterwards, questions can be written in the chat of the main Zoom room. Please tag questions related to lecture 1 with L1, questions related to lecture 2 with L2 and lecture 3 with L3. Moderators can only choose a limited number of questions to be discussed at the round table discussion. This session also povides the opportunity to establish contacts that can be continued using the private chat. Networking is an important tool not only in science.

Direct alpha-capture measurement of the 13N(α,p)16O reaction using the MUlti-Sampling Ionization Chamber (MUSIC) relevant for Type Ia supernovae

• Heshani Jayatissa (Argonne National Laboratory, United States)

Room: virtual The 13N(α,p)16O reaction has been recently found to have a significant impact in the estimated high yields of Carbon-13 during the ingestion of hydrogen into the helium shell of massive stars during the shock propagation of a core-collapse supernovae. The rate of this reaction determines the amount of Nitrogen-13 that can β-decay, producing Carbon-13. The reaction rate of the inverse reaction 16O(p,α)13N also plays a role in the creation of Carbon-12 by oxygen burning at high proton abundances via 16O(p,α)13N(γ,p)12C, which in turn affects the abundances of argon and calcium in type Ia supernovae nucleosynthesis. There are only very few experimental data available for the 13N(α,p)16O reaction and the rate of this reaction is not well-constrained. A direct measurement of the 13N(α,p)16O reaction was performed using a 30-MeV secondary beam of Nitrogen-13 from the Argonne In-Flight Radioactive Ion Separator (RAISOR) and the active-target detector MUSIC at Argonne National Laboratory. Preliminary results from this measurement will be discussed.

Moderated questions

• Ann-Cecilie Larsen (University of Oslo, Norway)

Room: virtual

Neutron-capture rates in massive stars: relevance for cosmochemistry

• Hannah Elisabeth Brinkman (Konkoly Observatory, Hungary)

Room: virtual Massive stars eject the products of their nuclear burning into the interstellar medium via stellar winds and supernova explosions. However, these yields are highly dependent on the nuclear reaction rates we implement in our models. We have analysed two science cases for which neutron-capture rates might make a significant impact on the results. The first is that of Chlorine-36 and Calcium-41. Both these isotopes are radio-active and were present in the early Solar System as inferred from meteoritic data. With the current reaction rates implemented in the JINA-reaclib, we determined that to better match the early Solar System abundances with our wind yields, we need either more Chlorine-36 or less Calcium-41, or a combination of the two options. One way to achieve this by testing different values of the main neutron-capture rates responsible of the destruction of the two isotopes in the stellar interior. Our simple tests show that decreasing the Chlorine-36(n,p) rate has little impact on the match with the early Solar System, while increasing the Calcium-41(n,alpha) rate leads to a better match, though there is still a discrepancy in the delay time between these two isotopes of a factor up to 3 derived from these two isotopes, from their wind ejection to the formation of the first solids in the Solar System. The second case where neutron-capture rates have an impact, is that of the production of Chromium-53,54, relative to Chromium-52, and of Titanium-50, relative to Titanium-48, in supernova progenitors. Predicted isotopic ratios of Chromium and Titanium can be used to determine the region of the star from which stardust chromite grains could have originated and the isotopic ratios indicated above are mainly influenced by neutron captures. Therefore, we preformed tests to vary these rates and determine their potential impact on the ratios, which allowed us to determine within nuclear physics uncertainties that the regions of massive stars from which the grains formed could have been the He and the C-shells. Ourwork demonstrates that new experimental determinations of the neutron-capture cross sections discussed above are needed to address cosmochemistry problems.

Moderated questions

• Ann-Cecilie Larsen (University of Oslo, Norway)

Room: virtual

Round table discussion Room: virtual Questions that were compiled in the chat after during lectures and breakout session will be answered and discussed