SNAQ October 2021

Europe/Brussels
virtual (online)

virtual

online

Konrad Schmidt (HZDR) , Olivier Sorlin (GANIL)
Description

ChETEC-INFRA SNAQs [snacks]

Schools on Nuclear Astrophysics Questions

Update: The SNAQ September 2021 was postponed to October 13 and the deadline for abstract submission was extended to September 29, 2021.

Question in October 2021: How to study stars from underground laboratories and deep-sea samples?

Scroll down for registration.

We highly encourage young scientists (master and PhD students, as well as young postdocs) to give scientific talks at this SNAQ related to the question above. If you are interested, please submit an abstract of your talk at the lower end of the registration form. Deadline for abstract submission is September 29, 2021. Successful candidates who give a talk after this competitive selection will receive the SNAQs Scientific Talk Award.

This is the 6th edition of a monthly, virtual school format discussing questions related to nuclear astrophysics.

Previous events:


We plan to organize a new event of SNAQs always on the 2nd Wednesday in each month with a break in summer (July to September). SNAQs will last about 3.5 hours, including breaks, with lectures and scientific talks around a given question in nuclear astrophysics. Lectures will be held by senior researchers and scientific talks preferably by young researchers, as master and PhD students. Further, SNAQs will 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 will join the community of schools related to nuclear astrophysics that partner with ChETEC-INFRA:

  • Carpathian Summer School of Physics (well established)
  • European Summer School on Experimental Nuclear Astrophysics (well established)
  • Intercontinental School on Nuclear Astrophysics (new)
  • International school on nuclear physics, neutron physics and applications (well established)
  • Nuclear Physics in Astrophysics School (new)
  • Rußbach School on Nuclear Astrophysics (well established)
  • School on observations and spectroscopic tools (new)

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 sixth SNAQ.


SNAQ September 2021 organizers SNAQs organizing committee
  • Konrad Schmidt (Helmholtz-Zentrum Dresden-Rossendorf, Germany)
  • Olivier Sorlin (Grand Accélérateur National d'Ions Lourds, France)
  • Rosanna Depalo (Università degli Studi di Milano, Italy)
  • Camilla Juul Hansen (Max Planck Institute for Astronomy Heidelberg, 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)
  • Mohamad Moukaddam (University of Strasbourg, France)
  • 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.

 

    • 13:45 14:00
      Zoom room available 15m
    • 14:00 14:10
      Welcome and Introduction 10m
      Speaker: Konrad Schmidt (Helmholtz-Zentrum Dresden-Rossendorf, Germany)
    • 14:10 14:20
      Russbach School on Nuclear Astrophysics 10m

      Introduction of the annual winter school and invitation to the Russbach School on Nuclear Astrophysics from March 13 to 19, 2022.
      https://events.hifis.net/e/russbach2022

      Speaker: Olivier Sorlin (Grand Accélérateur National d'Ions Lourds, France)
    • 14:20 15:00
      Why to study stars underground? 40m

      First lecture

      Speaker: Rosanna Depalo (Università degli Studi di Milano, Italy)
    • 15:00 15:10
      Moderated questions 10m
      Speaker: Konrad Schmidt (Helmholtz-Zentrum Dresden-Rossendorf, Germany)
    • 15:10 15:25
      Coffee break and breakout session 15m

      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.

    • 15:25 16:05
      How to study stellar explosions with deep-sea sediments and ocean crust? 40m

      Second lecture

      Speaker: Jenny Feige (Technische Universität Berlin, Germany)
    • 16:05 16:15
      Moderated questions 10m
      Speaker: Olivier Sorlin (Grand Accélérateur National d'Ions Lourds, France)
    • 16:15 16:30
      Coffee break and breakout session 15m

      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.

    • 16:30 16:45
      Measurements of 3He(α,γ)7Be γ-ray angular distribution at Felsenkeller shallow underground laboratory 15m

      Scientific talk

      The 3He(α,γ)7Be reaction plays a significant role in Big Bang nucleosynthesis, as well as solar fusion processes. Furthermore it affects the predicted solar 7Be and 8B neutrino fluxes as well as the nucleosynthesis of primordial 7Li. A measurement of the angular distribution of the prompt gamma rays may enable a better comparison between several experimental data sets at E = 0.7 - 1.3 MeV and a unique data set from the LUNA collaboration at E = 0.09 MeV - 0.13 MeV. Therefore the 3He(α,γ)7Be reaction is currently being studied with the 5MV Pelletron accelerator at the Felsenkeller shallow underground facility. The long-term focus lies on the measurement of the gamma ray angular distribution between 0.5 and 1.3 MeV in center of mass. In addition to this inbeam-analysis, the activated 7Be samples are counted offline on a counting setup, which was recently installed underground. This setup contains a HPGe detector with a relative detection efficiency of 163% in a sophisticated shielding consisting of active and passive components. First results of this ongoing campaign will be summarized.

      Speaker: Steffen Turkat (Technische Universität Dresden)
    • 16:45 16:50
      Moderated questions 5m
      Speaker: Marcel Heine (Hubert Curien Pluridisciplinary Institute, France)
    • 16:50 17:05
      Single Atom Counting of Stellar and r-Process Nuclei in Time-Resolved Deep-Sea Archives 15m

      Scientific talk

      Stars are the major element factories in the universe. In 1999, live supernova Fe-60 (2.6 Myr half-life) was detected in a deep-sea ferromanganese crust indicating the accumulation of supernova dust on Earth about 2 million years ago. This was followed by several projects reinforcing the initial evidence for a global influx of supernova Fe-60. Recently, a much younger continuous influx was found in Antarctic snow and in deep-sea sediments and an older peak around 6 to 8 Myr in deep-sea crusts. In contrast to the well-known production mechanism and synthesis site of Fe-60, the long-lived plutonium isotope Pu-244 (80 Myr half-life) is a pure r-process nucleus. The nucleosynthesis site for the astrophysical r-process is still debated in the astrophysics community. Potential candidates involve rare supernovae and neutron star mergers. To date no evidence was presented that would point to an exclusive r-process site and combinations of different sites are considered. Experimentally, we can search for Pu-244 signatures in samples with known Fe-60 signatures to test for either common influx patterns or independent Pu-244 influxes disentangled from stellar Fe-60. Accordingly, this information provides a unique and direct experimental approach for identifying the production site of the heavy elements. Based on the recent publication of the first detection of interstellar Pu-244 in a ferromanganese crust with a time resolution of 4.5 Myr (integrating over much shorter Fe-60 influxes), we are now working on a highly time-resolved profile of Fe-60 and Pu-244 in the large ferromanganese crust VA13/237KD. This direct experimental input will further constrain models for r-process nucleosynthesis in the galaxy. The recently determined profile of Fe-60 clearly shows two influxes, one at 2 Myr, the other at 7 Myr, confirming and refining previous results. Preliminary data on Pu-244 and an outlook for future measurement campaigns will be given.

      Speaker: Dominik Koll (Australian National University, Australia)
    • 17:05 17:10
      Moderated questions 5m
      Speaker: Livius Trache (Horia Hulubei National Institute for Physics & Nuclear Engineering, Romania)
    • 17:10 17:30
      Round table discussion 20m

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