SNAQ February 2022

online (virtual)



Sara Palmerini (INFN Perugia & University of Perugia, Italy), Konrad Schmidt (HZDR)


Schools on Nuclear Astrophysics Questions

Question in February 2022: How to model a star in your laptop?

Update: Below, all talks are available as PDF for download.

Update: Congratulation to the 2 winners of our SNAQs Scientific Talk Award in recogrecognition and appreciation for giving a scientic talk at the February 2022 edition of SNAQs:

  • Federico Rizzuti (Keele University, United Kingdom)
  • Teodora Andreea Madgearu (Extreme Light Infrastructure, Romania)

And thanks to all other applicants who submitted an abstract.

This is the 10th edition of a monthly, virtual school format discussing questions related to nuclear astrophysics.

Previous events:
Next event:  

A new event of SNAQs is organized always on the 2nd Wednesday in each month with a break in summer. SNAQs last about 3.5 hours, including breaks, with lectures and scientific talks around a given question in nuclear astrophysics. Lectures are held by senior researchers and scientific talks preferably by young researchers, as master and PhD students. Further, SNAQs put a special focus on the interaction between participants to allow young scientists networking even if traveling to schools, workshops and conferences is not an option.

SNAQs join the community of schools related to nuclear astrophysics that partner with ChETEC-INFRA:

The aim of this community is to give all students and young researchers the same, multidisciplinary knowledge about nuclear astrophysics. SNAQs will support this idea and strengthen the community of schools by providing a frequent lecture series to train and educate the next generation of scientist with knowledge across the three types of infrastructures used by nuclear astrophysicists:

  • astronuclear laboratories supplying reaction data,
  • supercomputer facilities performing stellar structure and nucleosynthesis computations, and
  • telescopes and mass spectrometers collecting elemental and isotopic abundance data.

Those infrastructures are networked by ChETEC-INFRA, Chemical Elements as Tracers of the Evolution of the Cosmos - INFRAstructures for Nuclear Astrophysics, a new European starting community of 32 partner institutions.

We are looking forward to meet you at the 9th SNAQ.

SNAQ February organizers SNAQs organizing committee
  • Sara Palmerini (University of Perugia, Italy)
  • Rosanna Depalo (Università degli Studi di Milano, Italy)
  • Camilla Juul Hansen (TU Darmstadt, Germany)
  • Marcel Heine (Hubert Curien Pluridisciplinary Institute, France)
  • Ann-Cecilie Larsen (University of Oslo, Norway)
  • Andreas Korn (Uppsala University, Sweden)
  • Arūnas Kučinskas (Vilnius University, Lithuania)
  • Sara Palmerini (University of Perugia, Italy)
  • Gianluca Pizzone (Laboratori Nazionali del Sud, Italy)
  • Konrad Schmidt (Helmholtz-Zentrum Dresden-Rossendorf, Germany)
  • Olivier Sorlin (Grand Accélérateur National d'Ions Lourds, France)
  • Livius Trache (Horia Hulubei National Institute for Physics & Nuclear Engineering, Romania)
  • Aurora Tumino (Kore University of Enna, Italy)

Guidelines for participants of SNAQs

Please, …
… rename yourself in the Zoom sessions to match your registration name and institution – this will serve as your “nametag”.
… mute your microphone during talks.
… use the public chat only for questions related to the lecture; for discussions, please use the private chat.
… write your questions in the chat – due to the high number of participants, a moderator will read a selection of questions but can choose a limited number only.
… use breakout rooms to talk and chat to each other in smaller groups. Breakout rooms will be available during coffee breaks and participants can choose rooms freely.
… behave professionally and respectfully.
… follow ethical standards as professional integrity and honesty.
… foster a welcoming and inclusive work environment.

    • 1:45 PM 2:00 PM
      Zoom room available 15m
    • 2:00 PM 2:05 PM
      Welcome and Introduction 5m
      Speaker: Konrad Schmidt (Helmholtz-Zentrum Dresden-Rossendorf, Germany)
    • 2:05 PM 2:50 PM
    • 2:50 PM 3:00 PM
      Moderated questions 10m
      Speaker: Sara Palmerini (INFN Perugia & University of Perugia, Italy)
    • 3:00 PM 3:45 PM
      How to make elements in my computer 45m
      Speaker: Marco Pignatari (Konkoly Observatory, Hungary)
    • 3:45 PM 3:55 PM
      Moderated questions 10m
      Speaker: Rosario Gianluca Pizzone (Laboratori Nazionali del Sud, Italy)
    • 3:55 PM 4:15 PM
      Coffee break and breakout session 20m

      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 and questions related to lecture 2 with L2. 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.

    • 4:15 PM 4:25 PM
      Nuclear Physics in Astrophysics X (NPAX) conference and school 10m

      Invitation to Nuclear Physics in Astrophysics X (NPAX) conference (Sep 5 to 9, 2022) and school (Aug 29 to Sep 2, 2022)

      Speaker: Alberto Mengoni (ENEA Bologna and INFN, Sezione di Bologna, Italy)
    • 4:25 PM 4:40 PM
      3D hydrodynamics simulations of massive stars with the PROMPI code 15m

      The evolution of massive stars is deeply affected by uncertainties related to multi-dimensional processes that take place in stellar interiors (e.g. convection, rotation, magnetic activity). However, it is not computationally possible to simulate the entire lifetime of a star while also following its fluid motions explicitly. For this reason, 3D hydrodynamics simulations are used to support 1D stellar evolution codes by reproducing on a short timescale (minutes or hours) realistic 3D processes. In this talk, I will present the multi-dimensional hydrodynamics code PROMPI and results coming from a new set of high-resolution simulations of the neon-burning shell in a massive star, focusing on the interplay between nuclear burning and convection, as well as discussing the impacts of different resolutions and nuclear rate boosting on the results. This work was done in collaboration with Cyril Georgy, Raphael Hirschi, and David Arnett.

      Speaker: Federico Rizzuti (Keele University, United Kingdom)
    • 4:40 PM 4:45 PM
      Moderated questions 5m
      Speaker: Andreas Korn (Uppsala University, Sweden)
    • 4:45 PM 5:00 PM
      Direct measurement of the 19F(p,α)16O reaction 15m

      The 19F(p,α)16O reaction is important for understanding the fluorine abundance in the outer layers of asymptotic giant branch (AGB) stars and it might also play a role in hydrogen-deficient post-AGB star nucleosynthesis. Up to now, theoretical models overproduce F abundances in AGB stars with respect to the observed values, thus calling for further investigation of the reactions involving fluorine. Indeed, in the last years, new direct and indirect measurements improved significantly the knowledge of the 19F(p,α0)16O cross section at deeply sub-Coulomb energies (below 0.8 MeV). Nevertheless, those data are larger by a factor of about 1.4 with respect to the previous data reported in the NACRE compilation in the energy region 0.6-0.8 MeV. In order to solve these discrepancies, we present here a direct experiment performed at INFN-LNS using a silicon strip detector array (LHASA - Large High-resolution Array of Silicon for Astrophysics). Our results clearly confirm the trend of the latest experimental data in the energy region of interest. The 19F(p,α)16O reaction rate is the sum over the (p,α0), (p,απ) and the (p,αγ) channels. While the (p,α0) rate is well constrained by the present existing data, down to the lowest energies, almost nothing is known from experiments on the (p,απ) and (p,αγ) rates. Despite its importance, the S-factors and the branching ratio between the α0, απ and αγ outgoing channels in the 19F(p,α)16O reaction are still largely uncertain at astrophysical energies, emphasizing the need for better measurements. Thus, a direct measurement using the new detector, ELISSA (Extreme Light Infrastructure – Silicon Strip Array), coupled with LHASA will be performed in September 2022 at IFIN-HH. This setup is allowing us to discriminate the (p,απ) and (p,αγ) reaction rates at very low energies.

      Speaker: Teodora Andreea Madgearu (Extreme Light Infrastructure, Romania)
    • 5:00 PM 5:05 PM
      Moderated questions 5m
      Speaker: Andreas Korn (Uppsala University, Sweden)
    • 5:05 PM 5:30 PM
      Round table discussion 25m

      Questions that were compiled in the chat during and after lectures and the breakout session will be answered and discussed.