registrants book - tum physikdepartment (indico)...dr. domingo garcía-senz #39 registration details...

16th Rußbach School on NuclearAstrophysics, March 2019

Registrants Book

https://indico.ph.tum.de/e/russbach2019

Table of contents

Ani Aprahamian 1.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Massimo Barbagallo 2.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Hannah Brinkman 3.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Silvio CHERUBINI 4.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Sandrine Courtin 5.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Borbála Cseh 6.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Roland Diehl 7.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Brian Fields 8.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Domingo García-Senz 9.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Felix Heim 10.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Wolfgang Hillebrandt 11.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Heshani Jayatissa 12.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Jordi Jose 13.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Armel KAMENYERO 14.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Kratz Karl-Ludwig 15.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Heamin Ko 16.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Marvin Körschgen 17.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Louis Lalanne 18.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Manuel Linares 19.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Matej Lipoglavsek 20.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Nan Liu 21.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Martin Müller 22.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Yuliya Mutafchieva 23.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Sara Palmerini 24.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Ferdinando Patat 25.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Moritz Pleintinger 26.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Madalina Ravar 27.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Ante Ravlic 28.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

i

Stephan Rosswog 29.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

stefania salvadori 30.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Hendrik Schatz 31.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Gerhard Schmidt 32.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Konrad Schmidt 34.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Philipp Scholz 35.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Alexandra Spiridon 36.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Iuliana Madalina Stanciu 37.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Ionut-Catalin Stefanescu 38.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Zhivko Stoyanov 39.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Oscar Straniero 40.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Mihai Straticiuc 41.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Jose Luis Tain 42.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Reto Trappitsch 43.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Dana Tudor 44.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Louis Wagner 45.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Michael Wiescher 46.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Andrés Yagüe López 47.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Yuta Yamazaki 48.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Azzurra Zucchini 49.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

ii

Prof. Ani Aprahamian #14

Registration details

Registration date: 12 Dec 2018, 19:07Registration state: Completed

Personal Data

Institution: Nuclear Science Laboratory, University of Notre Dame

Abstract Submission

Write your title and abstract here: Nuclear experiments and the neutron starmerger

16th Rußbach School on Nuclear... / Registrants Book Ani Aprahamian

Page 1 Tuesday 12 March 2019

Dr. Massimo Barbagallo #55


Registration date: 31 Jan 2019, 12:06Registration state: Completed

Personal Data

Institution: CERN

Abstract Submission

Write your title and abstract here: High intensity neutron beams andNucleosynthesis studies at CERN

16th Rußbach School on Nuclear... / Registrants Book Massimo Barbagallo


Ms. Hannah Brinkman #23



Personal Data

Institution: Konkoly Observatory

Abstract Submission

Write your title and abstract here: Title: Al26 yields from massive binary starsAbstract: There is strong evidence for the presence of Al26 in the early solarsystem, a radioactive isotope with a half life time of about 7.2*10^5 years, which isalso detected in the Galaxy via gamma-ray observations. However, while it isknown that Al26 is produced in stars, many uncertainties are left in the productionsites and the nuclear physics input. Past research has focused mostly on explosiveyields of Al26 from single stars and some wind yields. My research focuses on theyields from massive star winds, 20-60Msun, and the yields from non-conservativemass transfer in binary systems with the same primary masses. In my talk, I willshow the first results of my research.

16th Rußbach School on Nuclear... / Registrants Book Hannah Brinkman


Prof. Silvio CHERUBINI #49



Personal Data

Institution: University of Catania and INFN - Laboratori Nazionali del Sud

Abstract Submission

Write your title and abstract here: Trojan Horse Method: basic ideas and recentresults

16th Rußbach School on Nuclear... / Registrants Book Silvio CHERUBINI


Prof. Sandrine Courtin #38



Personal Data

Institution: IPHC and University of Strasbourg

Abstract Submission

Write your title and abstract here: The 12C+12C fusion reaction at astrophysicalenergies

16th Rußbach School on Nuclear... / Registrants Book Sandrine Courtin


Mrs. Borbála Cseh #22



Personal Data

Institution: Konkoly Thege Miklós Astronomical Institute, Research Centre forAstronomy and Earth Sciences, Hungarian Academy of Sciences

Abstract Submission

Write your title and abstract here: The Composition of Barium stars and thes-Process in AGB Stars Barium stars belong to a binary system where thecompanion star has evolved through the AGB phase and transferred elementsheavier than Fe produced by the slow neutron-capture process onto the secondarystar, which is now observed. A new large set of homogeneous high resolutionspectra of Ba stars makes it now possible to meaningfully compare theobservational data with different AGB models and with other observations. The Bastar data shows an incontestable increase of the hs-type/ls-type element ratio (forexample, Ce/Y) with decreasing the metallicity. The trend in the Ba starobservations is predicted by non-rotating AGB models where 13C is the mainneutron source. Observations of the cores of red giant stars and of white dwarfs(the ancestors and the progeny of AGB stars, respectively) inferred viaasteroseismology from Kepler observations show low core rotational velocities,which is in agreement with the results from the Ba star data and may derive fromcoupling between the core and the envelope.

16th Rußbach School on Nuclear... / Registrants Book Borbála Cseh


Prof. Roland Diehl #37



Personal Data

Institution: MPE Garching

Abstract Submission

Write your title and abstract here: Observations of cosmic nuclei thoughgamma-ray line spectroscopy

16th Rußbach School on Nuclear... / Registrants Book Roland Diehl


Brian Fields #43



Personal Data

Institution: University of Illinois

Abstract Submission

Write your title and abstract here: When Stars Attack! Near-Earth SupernovaeRevealed by Geological and Lunar 60Fe Radioisotopes Supernovae are majorengines of nucleosynthesis, and create many of the elements essential for life. Yetthese awesome events take a sinister shade when they occur close to home,because an explosion very nearby would pose a grave threat to Earthlings. We willshow how radionuclides produced by supernovae can reveal nearby events in thegeologic past, and we will highlight isotopes of interest. In particular, acceleratormass spectrometry has detected live 60Fe globally in deep-ocean material, and inlunar samples. We will review astrophysical 60Fe production sites and show thatthe data demand that one or more core-collapse supernovae exploded near theEarth about 3 Myr ago, and explain how debris from the explosion was transportedto the Earth as a "radioactive rain." The 60Fe measurements represent a new toolfor nuclear astrophysics: we can now use sea sediments and lunar cores astelescopes, probing supernova nucleosynthesis and possibly even indicating thedirection towards the event(s). We will close by reviewing recent work showing thatan explosion so close was probably a "near-miss" that exposed the biosphere tointense and possibly harmful ionizing radiation. I could also speak on Big BangNucleosynthesis, if that would be helpful to the school. If so can provide a title andabstract. But as suggested by the organizers I'd be particularly eager to talk aboutnear-earth supernovae as noted above.

16th Rußbach School on Nuclear... / Registrants Book Brian Fields


Dr. Domingo García-Senz #39



Personal Data

Institution: Universitat Politècnica de Catalunya

Abstract Submission

Write your title and abstract here: Title: The Single Degenerate channel to TypeIa supernova explosions: the modeler point of view. Abstract. The explosion of awhite dwarf, triggered by the accretion of hydrogen from a nearby non-degeneratestar, has traditionally been considered the dominant production channel for Type IaSupernova. Such scenario is, however, not the preferred one at present time but itstill could represent a non-negligible fraction of the total SNe Ia sample. In thislecture I will review the pros and cons of the different proposed models within thesingle degenerate (SD) paradigma, with especial emphasis in the hydrodynamicsimulations of these explosions. Results of a recent work analyzing the role ofrotation in the symmetry breaking of point-like triggered explosions will becommented at the end of the talk.

16th Rußbach School on Nuclear... / Registrants Book Domingo García-Senz


Mr. Felix Heim #26



Personal Data

Institution: University of Cologne

Abstract Submission

Write your title and abstract here: TITLE: Insights into the statistical$\gamma$-decay behaviour of $^{108}$Cd via radiative proton capture Abstract:For many nucleosynthesis processes in various astrophysical scenarios crosssections and reaction rates need to be predicted by statistical model calculations.One of those processes is the $\gamma$ process, which plays an important role inthe nucleosynthesis of the majority of the $p$ nuclei. The calculated valuesdepend heavily on nuclear physics input-parameters like nuclear level densities(NLD), $\gamma$-ray strength functions ($\gamma$-ray SF) and nucleon+nucleusoptical model potentials (OMPs). Precise cross-section measurements atastrophysical energies can be used to test and validate microscopic theoreticalapproaches for these nuclear physics models. For this reason, total and partialcross-sections of the $^{107}$Ag(p,$\gamma$)$^{108}$Cd reaction weremeasured via the in-beam method at the high-efficiency HPGe $\gamma$-rayspectrometer HORUS at the University of Cologne. Proton beams with energiesbetween 2.0 and 5.0 MeV were provided by the 10 MV FN-Tandem accelerator.The NLD and $\gamma$-ray SF in $^{108}$Cd were extracted in a way that theydo not only agree with the total and partial cross-section results but also preservephysical reliability.\\ This method will be applied on the$^{109}$Ag(p,$\gamma$)$^{110}$Cd and $^{93}$Nb(p,$\gamma$)$^{94}$Moreactions as well, for which experiments have already been performed andpreliminary results will be presented. Supported by the DFG (ZI 510/8-1) and the"ULDETIS" project within the UoC Excellence Initiative institutional strategy.

16th Rußbach School on Nuclear... / Registrants Book Felix Heim


Prof. Wolfgang Hillebrandt #6


Registration date: 30 Oct 2018, 15:50Registration state: Completed

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Institution: Max-Planck-Instutute for Astrophysics

Abstract Submission

Write your title and abstract here: Measuring the expansion rate of the Universe:Is 'Hubble's constant' constant? Although systematic uncertainties may limit theaccuracy of thermonuclear (Type Ia) supernovae as distance indicators forcosmology, they are at present the best tools to determine relative distances in theUniverse. However, an extremely important question is: Can we determineaccurate absolute distances also, reflected in the uncertainty of today's expansionrate of the Universe, the Hubble constant H0. In fact, the present 5% discrepancyin H0 determinations between the cosmic microwave background and Type Iasupernovae either points at additional cosmological components or errors in themeasurements, and this uncertainty on H0 is a severe limitation on an accuratedetermination of most other cosmological parameters. In this talk we will discussseveral promising ways to obtain high-precision measurements of H0 in the nearfuture.

16th Rußbach School on Nuclear... / Registrants Book Wolfgang Hillebrandt


Ms. Heshani Jayatissa #8


Registration date: 14 Nov 2018, 17:38Registration state: Completed

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Institution: Texas A&M; University Cyclotron Institute

Abstract Submission

Write your title and abstract here: Sub-Coulomb (6Li,d) alpha-transfer techniquefor the reaction rate study of the 22Ne(alpha,n) alpha-capture reaction. The22Ne(alpha,n) reaction is a very important neutron source reaction for the slowneutron capture process (s-process) in asymptotic giant branch stars. These directmeasurements are very difficult to carry out at the energy regimes of interest forastrophysics (Gamow energies) due to the extremely small reaction cross section.The large uncertainties introduced when extrapolating direct measurements at highenergies down to the Gamow energies can be overcome by measuring theAsymptotic Normalization Coefficients (ANC) of the relevant states usingalpha-transfer reactions at sub-Coulomb energies to reduce the modeldependence. The study of the 22Ne(6Li,d) and 22Ne(7Li,t) reaction was carriedout at the Cyclotron Institute at Texas A&M; University. The alpha-ANCmeasurements for the near alpha-threshold resonances of 26Mg provideconstraints for the 22Ne(alpha,n) reaction rate. The effect of this reaction rate onthe final abundances of the s-process isotopes will be discussed.

16th Rußbach School on Nuclear... / Registrants Book Heshani Jayatissa


Prof. Jordi Jose #56



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Institution: Universitat Politecnica de Catalunya

Abstract Submission

Write your title and abstract here: "12321 Models of Classical Novae" Abstract.Classical novae are thermonuclear explosions that take place in the envelopes ofaccreting white dwarfs in stellar binary systems. The material piles up underdegenerate conditions, driving a thermonuclear runaway. The energy released bythe suite of nuclear processes operating at the envelope heats the material up topeak temperatures of (100 - 400) MK. During these events, about 10-3 - 10-7 solarmasses, enriched in CNO and, sometimes, other intermediate-mass elements(e.g., Ne, Na, Mg, Al) are ejected into the interstellar medium. In this talk, wepresent new multidimensional simulations of mixing at the core-envelope interfaceduring classical novae, for different masses and chemical compositions of theunderlying white dwarf. Accretion of solar composition material onto CO and ONewhite dwarfs was initially computed with the 1D hydrodynamic code SHIVA. Whenthe temperature at the core-envelope interface reached 100 MK, the structure wasmapped onto a 3D cartesian grid that was subsequently followed with themultidimensional code FLASH ("1 to 3" or "123" models). In this multidimensionalframework, Kelvin-Helmholtz instabilities can naturally lead to self-enrichment ofthe accreted envelope with material from the underlying white dwarf at levels thatagree with observations.The final fate of the runaway was followed with SHIVA,remapping the 3D structure onto a 1D grid ("3 to 1" or "321" models), which allowsthe investigation of the dynamic stages of the explosion. New nucleosynthesisresults, with particular emphasis on the production of 7Li, recently reported fromobservations of novae, will also be presented.

16th Rußbach School on Nuclear... / Registrants Book Jordi Jose


Mr. Armel KAMENYERO #40



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Institution: GANIL

Abstract Submission

Write your title and abstract here: "Spherical, cluster and haloes structures in12Be probed by 13(-p) reaction at GSI"

16th Rußbach School on Nuclear... / Registrants Book Armel KAMENYERO


Prof. Kratz Karl-Ludwig #2



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Institution: Fachbereich 09, University of Mainz

Abstract Submission

Write your title and abstract here: Cosmochemistry - r-Process

16th Rußbach School on Nuclear... / Registrants Book Kratz Karl-Ludwig


Ms. Heamin Ko #57



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Institution: Soonsil University

Abstract Submission

Write your title and abstract here: Title : Neutrino self-interaction and MSWeffects on the supernova neutrino-process Abstract: In this study, we investigatethe neutrino process during supernova explosion. In supernova environment, theneutrinos propagate through electron and neutrino backgrounds. We apply thisneutrino oscillation effects on neutrino process in supernova 1987A model. Ourfocus is some elements, which are uniquely produced by neutrino-inducedreactions. The light element Li7 and B11 are mainly produced in He-layer, whilethe heavy elements such as 92Nb, 98Tc and 138La are produced in relative innerregion, i.e. O-Ne-Mg region. As a result, the effects of neutrino interaction withelectron and neutrino itself increase the abundances, because they produce higherenergy number of electron type neutrinos by changed flavor from mu and tau typeneutrinos.

16th Rußbach School on Nuclear... / Registrants Book Heamin Ko


Mr. Marvin Körschgen #29



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Abstract Submission

Write your title and abstract here: Title: Investigation of ($\alpha$,$\gamma$)reaction cross sections of ruthenium isotopes Photodesintegration networks areone of the main processes in the nucleosynthesis of p-nuclei. Especially($\gamma$,$\alpha$) reactions play a crucial role in the production of the heaviestp-nuclei $[$1$]$. Practically they are obtained by the measurement of inverse($\alpha$,$\gamma$) reaction cross sections at sub coulomb energies andstatistical model calculations. The latter requires fundamental knowledge of opticalmodel potentials (OMPs), nuclear level densities (NLDs) and the $\gamma$-raystrength functions ($\gamma$-ray SFs).\\ This talk will cover a project aiming tomeasure ($\alpha$,$\gamma$) reaction cross sections on ruthenium isotopesapplying the 4$\pi$ summing method $[$2$]$. The measurements take place at theDynamitron Tandem Laboratorium of the Ruhr-Universität Bochum, Germany,using a 12 by 12 inch NaI(Tl) crystal.\\ This work is supported by the DFG(ZI-510/8-1).\\ $[$1$]$ M. Arnould and S. Goriely, Phys. Rep. \textbf{384} (2003) 1.\\ $[$2$]$ A. Spyrou, H.W. Becker, A. Lagoyannis, S. Harrisopulos, and C. Rolfs,Phys. Rev. C \textbf{76} (2007) 1.

16th Rußbach School on Nuclear... / Registrants Book Marvin Körschgen


Mr. Louis Lalanne #24



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Institution: IPN Orsay

Abstract Submission

Write your title and abstract here: 36Ca studied through transfer reaction and itsrole in the proton capture 35K(p,γ)36Ca in X-ray bursts X-ray bursts arethermonuclear flashes occurring when a neutron star accretes matter from alow-mass main sequence star’s companion. For given conditions of temperatureand pressure in the accretion disc, the bursts are powered by triple-α reaction, αpprocess, followed eventually by rapid proton captures (rp). During the rp process,the 35K(p,γ)36Ca reaction is expected to play an important role in shaping theburst’s light curve [0]. This reaction mainly proceeds through the resonant captureto the (unbound) first 2+ state, whose energy relative to the 35K+p threshold, aswell as gamma and proton decay widths, are essential to determine its rate. Duringsummer 2018, an experiment to study 36Ca excited states and their decay modeshas been performed at GANIL. This nucleus was studied by means of the37Ca(p,d) and 38Ca(p,t) transfer reactions. Radioactive beams of 37Ca and 38Ca,produced with the LISE spectrometer, were tracked by two sets ofposition-sensitive detectors before being sent on a liquid hydrogen cryogenictarget of liquid H, in which (p,d) and (p,t) transfer reactions took place. 8 MUST2Silicon telescopes were used to identify and measure the energy and angle of lightparticles emitted at forward angles and an assembly of three detectors (ionizationchamber, drift chamber and plastic scintillator) was used to detect the transfer-likenuclei. During the analysis, states in 36Ca were selected by identifying a d or tparticle in MUST2, in case of a 37Ca or 38Ca incident beam, respectively, incoincidence with outgoing Ca or K nuclei, corresponding to states in 36Ca thatunderwent gamma or proton decay, respectively. With these data, the energy anddecay widths of the 2+ first excited state will be measured to be able to determinethe 35K(p,γ)36Ca cross section. Moreover, the study of 36Ca offers several otherscientific interests, such as the study of isospin symmetry breaking compared to itsmirror nucleus 36Si and the characterization of two-protons decaying states. In thispresentation, the physics motivation will be presented first, followed by theexperimental set-up and some preliminary results. [0] R.Cyburt and al. 2016, ApJ830, 55

16th Rußbach School on Nuclear... / Registrants Book Louis Lalanne


Dr. Manuel Linares #63


Registration date: 4 Feb 2019, 21:38Registration state: Completed

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Institution: UPC-GAA

Abstract Submission

Write your title and abstract here: Neutron star masses and radii: constraints onthe equation of state of ultradense matter. I will review our current knowledge ofthe masses and radii of neutron stars, obtained mostly from astronomicalobservations of binary pulsars. I will present some of the techniques that havebeen used to measure neutron star masses and radii for more than three decades,and mention the new constraints that come from gravitational wave astronomy. Iwill also discuss the implications of the most massive neutron stars for theequation of state at supra-nuclear densities.

16th Rußbach School on Nuclear... / Registrants Book Manuel Linares


Prof. Matej Lipoglavsek #13



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Institution: Jozef Stefan Institute

Abstract Submission

Write your title and abstract here: Nuclear reactions at low energies Electronscreening influences nuclear reactions at low energies both in the laboratory and inthe stars. However, the laboratory measurement show no resemblance to what wethink should be happening in the stars. I will present some of the problems and hintat possible solutions.

16th Rußbach School on Nuclear... / Registrants Book Matej Lipoglavsek


Dr. Nan Liu #21



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Institution: Washington University, St. Louis

Abstract Submission

Write your title and abstract here: Presolar Silicon Carbide Grains and TheirStellar Origins Condensates formed in dying stars prior to the solar systemformation, known as presolar grains, were identified in primitive meteorites formedin the solar system about 30 years ago based on their large isotopic deviationsfrom the solar system ratios. Despite of their tiny sizes (sub-μm to μm in size), thepresence of ancient stellar materials on Earth has allowed detailedcharacterization of their structural and isotopic compositions using a suite ofmodern microanalytical techniques with precisions that greatly surpass those ofthe most-up-to-date spectroscopic data. Among diverse presolar mineral phases,silicon carbide (SiC) has been most extensively studied because of its rarity in thesolar system and relatively easy separation from solar system material by aciddissolution. This talk will present an overview of different groups of presolar SiCgrains and their stellar origins based on recent results from multi-element isotopicanalyses of these grains. In particular, I will present multi-element isotopic data forpresolar 13C-rich (12C/13C≤10) grains and their stellar sources will be discussedby considering astronomical observations and nucleosynthetic model calculations.

16th Rußbach School on Nuclear... / Registrants Book Nan Liu


Mr. Martin Müller #28



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Abstract Submission

Write your title and abstract here: Title: Investigation of total cross sections ofthe $^{93}$Nb(p,$\gamma$)$^{94}$Mo reaction The nucleosynthesis of p-nuclei isan important field of research in the area of nuclear astrophysics and a lot ofquestions remain unanswered. One example is the observed relative abundanceof the $^{94}$Mo nucleus, which is higher than the predicted one by orders ofmagnitude. To extend experimental data, total cross sections of the$^{93}$Nb(p,$\gamma$)$^{94}$Mo reaction have been measured at three beamenergies between 3 MeV and 4.5 MeV. The measurements have been performedusing the HORUS $\gamma$-spectrometer consisting of up to 14 high puritygermanium detectors. The beam was provided by the 10 MV FN Tandemaccelerator, located at the University of Cologne's Institute for nuclear physics.\\Preliminary results and their comparison to Hauser Fesh\-bach statistical modelcalculations will be presented. \\ Supported by the DFG (ZI 510/8-1) and the"ULDETIS" project within the UoC Excellence Initiative institutional strategy. \\

16th Rußbach School on Nuclear... / Registrants Book Martin Müller


Ms. Yuliya Mutafchieva #51



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Institution: Institute for Nuclear Research and Nuclear Energy, BAS

Abstract Submission

Write your title and abstract here: Influence of the magnetic field on magnetarcrusts Magnetars exhibit some of the highest observed magnetic fields (of theorder of 10^15 G at their surface). The influence of the magnetic fields on theoutermost regions of these stars is discussed. The effects of the quantization ofelectron motion into Landau-Rabi levels on the crustal composition and equation ofstate are studied. The presented numerical results for both the outer and innercrusts were obtained using models based on the nuclear-energy density functionaltheory.

16th Rußbach School on Nuclear... / Registrants Book Yuliya Mutafchieva


Dr. Sara Palmerini #34



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Institution: Università degli Studi di Perugia & INFN Perugia

Abstract Submission

Write your title and abstract here: s-Processing from MHD-induced Mixing andIsotopic Abundances in Presolar SiC Grains In the past years the observationalevidence that s-process elements from Sr to Pb are produced by stars ascendingthe so-called Asymptotic Giant Branch (or AGB) could not be explained byself-consistent models, forcing researchers to extensive parameterizations. Thecrucial point is to understand how protons can be injected from the envelope intothe He-rich layers, yielding the formation of 13C and then the activation of the13C(α,n)16O reaction. Only recently, attempts to solve this problem started toconsider quantitatively physically-based mixing mechanisms. Among them, MHDprocesses in the plasma were suggested to yield mass transport through magneticbuoyancy. In this framework, we compare results of nucleosynthesis models forlow mass AGB stars (M≤3M⊙), developed from the MHD scenario, with the recordof isotopic abundance ratios of s-elements in presolar SiC grains, which wereshown to offer precise constraints on the 13C reservoir. We find that n-capturesdriven by magnetically-induced mixing can well account for the SiC data and thatthis is due to the fact that our 13C distribution fullfils the above constraints ratheraccurately. We show comparisons between model predictions and measurementsfor isotopes of Sr, Zr and Ba as representative examples of light and heavys-elements.

16th Rußbach School on Nuclear... / Registrants Book Sara Palmerini


Dr. Ferdinando Patat #64



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Institution: ESO

Abstract Submission

Write your title and abstract here: The progenitors of thermonuclearsupernovae: an observer's perspective In my lecture I will provide an updated andcomprehensive overview on the search for the progenitors of Type Ia Supernovae.I will go through all the methods and techniques deployed so far, illustrating prosand cons for each of them. I will then draw the status of affairs of this quest which,despite of great efforts, still remains without a final answer.

16th Rußbach School on Nuclear... / Registrants Book Ferdinando Patat


Mr. Moritz Pleintinger #41



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Institution: Max Planck Institute for Extraterrestrial Physics

Abstract Submission

Write your title and abstract here: Title: How Can We Learn about the Galaxy'sISM from Diffuse Radioactivities? Abstract: The interstellar medium in our Galaxyis understood to be of complex morphology and highly dynamic, far from a simplestate of pressure equilibrium. Commonly, 3D MHD simulations have beenexploited to get basic insights into the complexities of the ISM. Here,high-resolution simulations can trace physical processes down to the scales ofshocks from winds and explosions which inject turbulent energy into the ISM, whilestudies at the few-hundred to kpc scale adopt subgrid models for simulating theappearance of the Galaxy's ISM. Observations of the ISM are difficult due tobiases towards different phases of the ISM in each of the known gas tracers. Herewe exploit diffuse gamma-ray line emission, which complements suchobservations by a tracer of fresh nucleosynthesis ejecta, which is independentfrom gas density and temperature. The 1.8 MeV emission line from 26Al decay is akey tracer of ongoing nucleosynthesis and chemical enrichment in our Galaxy. Thisgamma-ray emission is prominent in the direction of individual massive star groupsand in the inner part of the Galactic plane. 26Al nuclei are ejected in strong stellarwinds (Wolf-Rayet phase) and supernova explosions. Because their half-life of~0.7 Myr is comparable to the crossing time of massive star ejecta insidesuperbubbles, the emission is closely connected to the dynamical properties ofmassive star groups and their surroundings. Investigating these circumstancesprovides a unique nexus between stellar physics and galactic evolution. Anoverview of recent 26Al observations performed with INTEGRAL/SPI and thecurrent understanding of feedback processes of massive OB associations on thesuperbubble scale will be given. This includes the description of recentchemodynamical simulations and our galactic population synthesis calculations aswell as how we can compare simulations with measurements. This opens thepossibility to validate 3D spatial distributions of the lage-scale 26Al emission and totest the underlying assumptions of stellar nucleosynthesis and feedback.

16th Rußbach School on Nuclear... / Registrants Book Moritz Pleintinger


Mrs. Madalina Ravar #19



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Institution: Institut für Kernphysik, Universität zu Köln

Abstract Submission

Write your title and abstract here: Preparations for studying the direct 3 decay ofthe 0+ 2 state in 12C with the Lund-York-CologneCalorimeter LYCCA(Lund-York-Cologne CAlorimeter), as part of the FAIR project is currently underconstruction, in the mean time a subarray is installed, com- missioned andexploited for experiments at the 10MV tandem accelerator of University ofCologne. The 0+2 state in 12C - the Hoyle state - and its direct decay into 3 alphasis planned to be studied via inelastic scattering on a car- bon target. The rst testexperiment employing the 12C( ; 0)12C� reaction at 21.35MeV center of massenergy, was carried out in order to study the feasi- bility of the demandingmeasurement. An array of 12 double-sided silicon strip detectors of highgranularity was employed and read out with newly developed AIDA (AdvancedImplantation Detector Array) electronics in order to search for the elusive 3 decaybranch. Results of the rst in-beam test measurement and plans for an improvedexperiment will be presented.

16th Rußbach School on Nuclear... / Registrants Book Madalina Ravar


Mr. Ante Ravlic #30



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Institution: Department of Physics, Faculty of Science, University of Zagreb

Abstract Submission

Write your title and abstract here: Electron capture rates at finite temperature Iam going to present my research on stellar electron capture rates at finitetemperature. Results are calculated using relativistic mean field theory withdensity-dependent meson interaction to obtain single-nucleon basis andcharge-exchange transitions are calculated using finite temperature relativisticrandom phase approximation. We present results for electron capture crosssections on even-even nuclei of iron, germanium and nickel at differenttemperatures. Capture rates are also calculated for iron-54,56, germanium-76,78,and nickel-62,64 for selected temperatures and stellar densities.

16th Rußbach School on Nuclear... / Registrants Book Ante Ravlic


Prof. Stephan Rosswog #65



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Institution: Department of Astronomy and Oskar Klein Centre, Stockholm

Abstract Submission

Write your title and abstract here: Lessons from first observed neutron starmerger On August 17, 2017 the era of multi-messenger astrophysics began: theLIGO-VIRGO detectors recorded, for the first time, the gravitational waves from aneutron star merger. Subsequently, telescopes around the world detected thecounterparts all across the electromagnetic spectrum. The combination ofgravitational and electromagnetic radiation from the same source has broughtmajor leaps forward on several decades-old puzzles, among many other resultsidentifying neutron star mergers as an important r-process source. I will reviewwhat (we think) we have learned and where the challenges lie for future work.

16th Rußbach School on Nuclear... / Registrants Book Stephan Rosswog


Dr. stefania salvadori #59



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Institution: University of Florence

Abstract Submission

Write your title and abstract here: CATCHING THE CHEMICAL SIGNATURESOF THE FIRST STARS The formation of the first stars brought the infant Universeout of the dark ages and changed its chemical composition by producing the firstheavy elements. In the Local Group, spectroscopic studies of ancient individualstars provide us with the unique opportunity to study the early phases of chemicalenrichment, and thus to look for the chemical signatures of the first stars. In thislecture, I will review the most recent observations for ancient metal-poor stars anddiscuss the implications for the properties of the first stars. I will show that some ofthe direct descendants of the first stars have been already observed. Finally, Ipresent theoretical predictions aimed at identifying many more of these rare stellarrelics to strongly constrain the Initial Mass Function of the first stars.

16th Rußbach School on Nuclear... / Registrants Book stefania salvadori


Hendrik Schatz #58



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Institution: Michigan State University

Abstract Submission

Write your title and abstract here: Rare Isotope Experiments in NuclearAstrophysics

16th Rußbach School on Nuclear... / Registrants Book Hendrik Schatz


Gerhard Schmidt #35



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Institution: Heidelberg University

Abstract Submission

Write your title and abstract here: Neutrons for Cosmochemistry: Activationanalysis at the Mainz TRIGA reactor - Identification of Impacting Asteroids GerhardSchmidt, Heidelberg University The Moon can provide insight into the earlydevelopment of the Earth, where the direct record of early evolution was destroyedby geological activity. During solidification of the Earth’s crust the surface wasexposed to a similar flux of impacting asteroids as the Moon. The Earth ImpactDatabase comprises a list of confirmed impact structures from around the world.To date, there are 190 confirmed impact structures in the database. To obtaininformation on the chemical composition of impacting asteroids, it is important toknow the relative abundances of Os, Ir, Ru, Pt, Rh and Pd in impact melts. Therefractory highly siderophile elements Os, Ru, Ir, and Rh are abundant in mostmeteorites but depleted in crustal rocks and therefore most reliable elements forprojectile identification. The Rh/Ir, Os/Ir and Ru/Ir ratios are particularly suitable fordistinguishing different types of meteorite projectiles. For example, magmatic ironmeteorites can be distinguished from non-magmatic iron meteorites by their lowerOs/Ir and higher Ru/Ir mass ratios (e.g., Schmidt et al. 1997). However,meteorite/target ratios are low if target rocks consist of mantle rocks. In this casePGE may enriched in impactites due to the relatively high abundances (ng/g level)in target rocks (e.g., Schmidt et al. 2000) to make the identification of the projectiletype quite difficult, if not impossible. The determination of these elements is adifficult challenge because of the low contents in the pg/g to ng/g range.Abundances of Os, Ir, Ru, Pt, Rh, Pd, Re and Au in impact melt samples andterrestrial rock samples were obtained by neutron activation analysis (NAA) at theInstitute for Nuclear Chemistry in Mainz from 1993 until 2005. The elementconcentrations were determined by using a nickel sulfide fire assay collectionprocedure on homogenized sample powders. The NAA procedure involved twoirradiations: a short irradiation for Rh and a long irradiation for other elements.Samples and Rh standards were first irradiated for 5 min at a thermal neutron fluxof 1.7 × 1012 neutrons cm-2 sec-1 in a hydraulic rabbit facility of the Mainz TRIGAReactor. After a delay time of 2 min, samples were counted for about 8 min. The104mRh (T1/2 = 4.41 min) γ-peak at 51 keV was used for the Rh-determination.After the completion of the first irradiation, samples were sealed together withchemical standards into clean capsules and irradiated for 12 hr in the core of thereactor at a flux of 4 × 1012 neutrons cm-2 sec-1. After the decay time of 16 hr,γ-spectra of the samples and standards were measured several times to determine109Pd, 188Re, 199Au (for Pt), 198Au, 192Ir, 191Os, and 103Ru. If no chemicalseparation of Ir from the matrix (especially Cr) was performed, only the 316 keVγ-line could be evaluated with NAA. The less sensitive 468 keV γ-line of 192Ir is

16th Rußbach School on Nuclear... / Registrants Book Gerhard Schmidt


not visible in the spectrum due to the increased compton background of the matrixelements. Also, the 316 keV γ-line cannot be completely resolved from the 320keV γ-line of 51Cr, so that part of Cr contributes to the Ir γ-line. This may result inseemingly higher Ir concentrations. However, if Ir and the other platinum groupelements are enriched from a homogenized sample powder and separated fromthe matrix by melt digestion, the 468 keV γ line can be evaluated, as was done atthe Institute for Nuclear Chemistry in Mainz. Thus (1) Ir can be detected muchmore sensitively over the 468 keV γ-line without (2) falsification of the analysis by51Cr. Today there are plenty of literature data on Ir, Os, Ru, Pt and Pd analyses ofrocks, impact melts and meteorites, but there are only few data on Rh, mainlybecause of the low concentrations and difficulties with mass spectrometricanalysis. In future studies, the database for these elements in impact melts,meteorites and terrestrial rocks has to be improved by neutron activation using ahigh neutron flux as neutron source. A melt digestion of sample material byinduction and subsequent determination of the elements with the CAMECA ims1280-HR ion microprobe in Heidelberg is also conceivable. High quality dataespecially of the mono isotopic element Rh might answer fundamental questions ofcosmochemistry and contribute to our understanding of the origin of the solarsystem and the processes involved in the formation and unique composition ofplanetary bodies. Schmidt, G., Palme, H., Kratz, K.-L. (1997) Highly siderophileelements (Re, Os, Ir, Ru, Rh, Pd, Au) in impact melts from three European craters(Sääksjärvi, Mien and Dellen): clues to the nature of the impacting bodies.Geochimica et Cosmochimica Acta 61, 2977-2987. Schmidt, G., Palme, H., Kratz,K.-L., Kurat G. (2000) Are highly siderophile elements (PGE, Re and Au)fractionated in the upper mantle of the earth? New results on peridotites fromZabargad. Chemical Geology 163, 167-188.

16th Rußbach School on Nuclear... / Registrants Book Gerhard Schmidt


Dr. Konrad Schmidt #33



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Institution: TU Dresden

Abstract Submission

Write your title and abstract here: X-ray bursts in the laboratory Type I X-raybursts take place on the surface of a neutron star accreting material from a binarycompanion. Important nuclear processes powering the X-ray burst are the triple-αreaction, the αp- and the rp-process. The Jet Experiments in Nuclear Structure andAstrophysics (JENSA) gas jet target enables the direct measurement of previouslyinaccessible reactions with radioactive beams provided by the rare isotopere-accelerator ReA3 at the National Superconducting Cyclotron Laboratory(NSCL), USA. JENSA is going to be the main target for the Recoil Separator forCapture Reactions (SECAR) at the Facility for Rare Isotope Beams (FRIB).

16th Rußbach School on Nuclear... / Registrants Book Konrad Schmidt


Dr. Philipp Scholz #36



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Institution: Institute for Nuclear Physics, University of Cologne

Abstract Submission

Write your title and abstract here: Radiative charged-particle reaction studies forthe nucleosynthesis of heavy isotopes — P. Scholz, F. Heim, M. Körschgen, J.Mayer, M. Müller, and A. Zilges — Institute for Nuclear Physics, University ofCologne Nuclear reaction cross sections are one of the main ingredients for theunderstanding of nucleosynthesis processes in stellar environments. For isotopessynthesized in the p- or r process [1,2], reaction rates on exotic nuclei are oftencalculated in the scope of the Hauser-Feshbach statistical model [3]. The accuracyof these reaction rates crucially depend on the uncertainties of nuclear-physicsinput-parameters like γ-ray strength functions, optical-model potentials, and leveldensities. The way to improve the reliability of statistical model calculations is toextend the available database for charged-particle induced reaction cross sectionsat low energies as well as using these data to study the underlying nuclear physicsproperties. This talk will summarize the different projects of our group, measuringproton and α-particle induced reactions in different mass regions and studying theγ-ray strength functions and α+nucleus opticalmodel potential. Supported by theDFG (ZI 510/8-1) and the "ULDETIS" project within the UoC Excellence Initiativeinstitutional strategy. [1] M. Arnould and S. Goriely, Phys. Rep. 384 (2003) 1. [2] M.Arnould et al., Phys. Rep. 450 (2007) 97. [3] W. Hauser and H. Feshbach, Phys.Rev. 87, 366 (1952).

16th Rußbach School on Nuclear... / Registrants Book Philipp Scholz


Dr. Alexandra Spiridon #45



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Institution: IFIN-HH

Abstract Submission

Write your title and abstract here: Transfer reactions as an Indirect Method inNuclear Astrophysics Alexandra Spiridon In this presentation, I will discuss the useof transfer reactions as an indirect method of determining information important fornuclear astrophysics. Specifically, I will focus on peripheral reactions and theiranalysis with the Asymptotic Normalization Coefficients (ANC) method. I willpresent results from related experiments that have been conducted at CyclotronInstitute, Texas A&M; University with focus on the Optical Model Parameters(OMP) obtained and the need of reliable calculations. Additionally, I will describethe improvements in the measured data that we obtained after upgrading thedetection system used and how this affects the OMP determination.

16th Rußbach School on Nuclear... / Registrants Book Alexandra Spiridon


Ms. Iuliana Madalina Stanciu #48



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Institution: Technische Universität München, Physik Department E68

Abstract Submission

Write your title and abstract here: To be discussed

16th Rußbach School on Nuclear... / Registrants Book Iuliana Madalina Stanciu


Mr. Ionut-Catalin Stefanescu #44



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Abstract Submission

Write your title and abstract here: “Complete spectroscopy” of 31S for nuclearastrophysics I.C. Stefanescu1,2, A.I. Chilug1,2, L. Trache1, A. Spiridon1, D.Tudor1,2, N. Mărginean1, A. Turturică1, L. Stan1, D. Filipescu1, N. Florea1, C.Costache1, S. Ujeniuc1, E. Radu1, C. Clisu1 1 Horia Hulubei National Institute forR&D; in Physics and Nuclear Engineering (IFIN-HH) 2 University of Bucharest,Doctoral School of Physics, Bucharest, Romania We study through gamma-rayspectroscopy methods the excited states in 31S at excitation energies up toEexc=7 MeV using equipment and alpha beam from the 9 MV tandem pelletron ofIFIN-HH Bucharest. The target used was a natural Si target. The measurementsare motivated by a nuclear astrophysics problem: the bottle-neck reaction in thechain of reactions in novae is 30P(p,g)31S, which is dominated by low lyingresonances. These are excited states in 31S, and the knowledge of these states’spectroscopy is insufficient at this time. Our goal is to complete data from othertypes of measurements with neutron-gamma coincidences. The reaction studiedwas 28Si(,n)31S and we used a detection system composed of 20 HPGedetectors and 5 neutron detectors in ROSPHERE, working in coincidence.Multiplicity M=2 of signals from all 25 detectors were collected and stored on disk.Due to neutron-gamma coincidences we were able to identify gamma rays abovethe proton separation energy in 31S (Sp=6.13 MeV) that go directly to g.s. of 31S,impossible to identify in a previous GAMMASPHERE measurement. Also, thewhole detection system behaved very well in what concerns the coincidencebetween gamma rays and neutrons.

16th Rußbach School on Nuclear... / Registrants Book Ionut-Catalin Stefanescu


Mr. Zhivko Stoyanov #52



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Institution: INRNE-BAS

Abstract Submission

Write your title and abstract here: Nuclear abundances in magnetar crusts Theobservations of the kilonova following the detection of gravitational waves fromGW170817, have confirmed the r-process triggered by the decompression ofejected crustal materials from binary neutron star mergers. R-processnucleosynthesis might also be possible due to the « magnetic eruption » inmagnetars. Part of the crust is ejected and the final abundance distributiondepends on the crustal composition. Using the latest experimental nuclear massdata supplemented with microscopic models, we show that the presence of a highmagnetic field can have a significant influence on the stratification of neutron-starcrusts and on the nuclear abundances of the different layers.

16th Rußbach School on Nuclear... / Registrants Book Zhivko Stoyanov


Dr. Oscar Straniero #9


Registration date: 21 Nov 2018, 10:01Registration state: Completed

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Institution: INAF

Abstract Submission

Write your title and abstract here: The mass of type II Supernova progenitors:hints for new physics? The progenitors of type II supernovae are red supergiants,i.e., massive stars in their late evolutionary phase. Recent surveys devoted to thesearch of SN progenitors have shown that no type II progenitors have mass above\sim 17-18 M_\odot, thus concluding that red supergiants with mass above thisthreshold, should directly collapse into a black hole, giving rise to a failedsupernova. It should be noted, however, that this colclusion is based on thetheoretical relation between progenitotor luminosity and initial mass, as derivedfrom current stellar models. We will show that this relation may be modified by theintroduction of new physics beyond the so-called "standard model". In particular,the possible production of weak interactive small particles, not included in thestandard model, may leads to an additional cooling of the stellar core during theadvanced burning phases and, in turn, to a lower progenitor luminosity.

16th Rußbach School on Nuclear... / Registrants Book Oscar Straniero


Dr. Mihai Straticiuc #42



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Abstract Submission

Write your title and abstract here: Small Particle Accelerators Used in NuclearAstrophysics (NA) Nowadays more than 30.000 particle accelerators operateworldwide in medicine, industry and basic research, while the small electrostaticmachines are in the range of a couple of hundreds. Most of the facilities builtaround a megavolt-infrastructure aim for applied research in solid-state physics,ion implantation or radiation hardness studies, but some of these MeV-rangeaccelerators proved to be excellent tools to use to obtain nuclear data needed tobetter understand the cosmogenic scenarios. In our institute, IFIN-HH inBucharest-Magurele, a 3 MV TandetronTM complemented by an ultra-lowbackground laboratory positioned inside of a salt mine open new opportunities, interms of sensitivity, for cross-section measurements at low energies. Wedemonstrate that with its stability, beam intensities and energy ranges the facility iscompetitive for nuclear astrophysics direct measurements with alpha and light ionbeams. A brief overview of the NA experiments performed by our group is alsopresented.

16th Rußbach School on Nuclear... / Registrants Book Mihai Straticiuc


Dr. Jose Luis Tain #17



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Institution: Instituto de Fisica Corpuscular, CSIC and University of Valencia

Abstract Submission

Write your title and abstract here: Title: Beta-delayed neutron measurements forastrophysics Abstract: Beta delayed-neutron emission occurs for sufficientlyneutron-rich nuclei when the decay populates states above the neutron separationenergy in the daughter nucleus. It was discovered in fission-products soon afterfission itself and it plays a key role in the control of nuclear reactors. Theimportance of this phenomenon in the description of rapid neutron capture (r-)processes occurring in explosive stellar scenarios with large neutron abundanceswas first pointed out in the seventies. The initial effect is the displacement to lowermasses of the distribution of elements synthetized along the r-process path. Inaddition the delayed neutrons reactivate the neutron capture reactions with theopposite effect. The computation of the final isotopic abundances requires theknowledge of decay properties for very neutron-rich nuclei that have eluded untilnow direct experimental investigation. The BRIKEN project was launched toextend significantly our knowledge of beta-delayed neutron emission probabilities(Pn) and half-lives (T1/2) into this region, combining the very high beam intensityachieved at the RIBF accelerator complex in RIKEN and the selection/identificationcapabilities for reaction products of the BigRIPS in-flight spectrometer, togetherwith state-of-the-art ion implant-and-decay detectors and moderated neutroncounters. The experimental program started in 2017 and envisages themeasurement of over 250 new beta-delayed neutron emitters, and 100 newhalf-lives covering the region from mass A~70 to A~200 with a direct impact inr-process nucleosynthesis calculations. In the presentation these aspects will behighlighted, the status of the experimental program reviewed and some initialresults will be shown.

16th Rußbach School on Nuclear... / Registrants Book Jose Luis Tain


Reto Trappitsch #25



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Institution: Lawrence Livermore National Laboratory

Abstract Submission

Write your title and abstract here: Laboratory studies of meteorites and presolargrains: Hands-on astrophysics Primitive meteorites, which formed early in theSolar System, can be used to study its original composition in terms of stable andradioactive nuclides. Furthermore, these meteorites contain stardust grains, whichrepresent the only natural samples available to probe nuclear astrophysics. Thesemicroscopic dust grains were produced in the death throes of stars and representindividual samples of stellar material. In my talk I will give an overview of meteoriteand presolar grain measurements and discuss how nuclear astrophysics andgalactic chemical evolution can be constrained from these analyses. For example,I will show how the initial abundance of 60Fe in the early Solar System, asmeasured in meteorites, can be used to constrain its birth environment.

16th Rußbach School on Nuclear... / Registrants Book Reto Trappitsch


Ms. Dana Tudor #46



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Institution: Horia Hulubei National Institute for R&D; in Physics and NuclearEngineering (IFIN-HH)

Abstract Submission

Write your title and abstract here: BEGA: a beta-gamma coincidence system tomeasure cross sections for short lived activities D. Tudor1;2, A. Spiridon1, L.Trache1, A.I. Chilug1;2, I.C. Stefanescu1;2, M. Straticiuc1, I. Burducea1 1IFIN-HH,Bucharest-Magurele, Romania 2Doctoral School of Physics, University ofBucharest, Romania [email protected] We proved that we can determineefficiently fusion ion-ion cross sections for nuclear astrophysics important reactionsat very low energies, under the Coulomb- barrier, by using the IFIN-HH 3 MVTandetron facility plus the ultra-low background laboratory placed in a salt mine.However this is usable for cases where activation leads to isotopes with life timessufficiently long for the transfer of the samples over 120 km. In order to addresscases where activities from isotopes that have shorter life times we designed, builtand tested a beta-gamma coincidence system (BEGA) which is meant for suchde-activation measurements. Therefore, the necessary background reduction ismade with beta-gamma coincidences. To test the system, targets of graphite werebombarded with 13C beam to produce 24Na. The decay of these samples weknow from the experiments we conducted in the last few years, so it was possibleto compare the BEGA detection system performances to the previous setup in thesalt mine. Results of the BEGA system tests will be presented.

16th Rußbach School on Nuclear... / Registrants Book Dana Tudor


Dr. Louis Wagner #4



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Institution: MSU/FRIB/NSCL/JINA-CEE

Abstract Submission

Write your title and abstract here: Title: First direct Measurement of the Reaction56Ni(α,p)59Cu for X-Ray Bursts Abstract: Sensitivity studies of Type I X-Ray burstmodels show that the reaction 59Cu(p,α)56Ni plays an important role to haveaccurate models to compare to observations of light curves. The cross section ofthe reaction can be constraint by the time-inverse reaction 56Ni(α,p)59Cu becauseit is predicted that only the ground state is populated at astrophysical energies. A56Ni radioactive beam experiment at the National Superconducting CyclotronLaboratory, East Lansing MI, USA measures this reaction in inverse kinematics forthe first time, using the JENSA helium gas jet target system. The reaction productsare detected by the superORRUBA silicon detector array and the GODDESSionization chamber. The talk covers experimental challenges and preliminary dataof the recent experiment.

16th Rußbach School on Nuclear... / Registrants Book Louis Wagner


Prof. Michael Wiescher #12



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Institution: University of Notre Dame

Abstract Submission

Write your title and abstract here: Nucleosynthesis in First Stars and the On-Setof Chemical Evolution: The first stars in our universe that emerged after the BigBang provide the environment for converting the primordial fuel of hydrogen,helium, and lithium isotopes into heavier elements. This conversion requires tobridge the mass A=5 and A=8 gaps of stable nuclei different reaction sequences togenerate for the first time 12C and 16O, the building blocks of all biological life inour universe. This talk will present the nuclear burning environment of these sitesand the reaction path that initiated the build-up of more complex nuclei, eventuallyleading to the elemental abundance distribution as observed today.

16th Rußbach School on Nuclear... / Registrants Book Michael Wiescher


Andrés Yagüe López #47



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Institution: Konkoly Observatory

Abstract Submission

Write your title and abstract here: TITLE: S-process nucleosynthesis for ATONABSTRACT: We present slow neutron-capture process (s-process)nucleosynthesis results for the stellar evolutionary code ATON for stars of 2, 3, 4,and 5 solar masses at solar metallicity. We then compare these results with thoseof other codes and observations. Finally, we briefly describe the effect that differentconvective and overshoot prescriptions have in our nucleosynthesis results.

16th Rußbach School on Nuclear... / Registrants Book Andrés Yagüe López


Mr. Yuta Yamazaki #53



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Institution: 1. Univ. of Tokyo, Graduate School of Science / 2.NationalAstronomical Observatory of Japan

Abstract Submission

Write your title and abstract here: Title: Cosmic evolution of r-processabundance pattern: Contribution from supernovae and neutron star mergers Thereare three possible astrophysical sites for the r-process nucleosynthesis; NDW-SN(neutrino driven winda from core-collapse supernovae(CCSNe)), MHDJ-SN(magnetohydrodynamically driven jets from CCSNe) and NSM (neutron starmerger). The GW170817/SSS17a, i.e. the neutron star merger, was an event ofthe century that opened a new window to multi-messenger astronomy andastrophysics. Optical and near-infrared emissions suggest that their total energyrelease is consistent with radiative decays of theoretical prediction of r-processnuclei although no specific r-process element was identified. However, NSM couldnot contribute to the very early Galaxy for cosmologically long merging time-scalefor too slow GW radiation. Nevertheless, NSM is still a one part of possibleexplanation for the present solar-system r-process abundance. On the other hand,CCSNe (both MHDJ- and NDW-SNe) are viable candidates for the r-process fromthe early phase of Galactic evolution. In particular, the MHDJ-SNe explain theuniversality in the observed elemental r-process abundance pattern in metal poorstars. We here propose a theoretical model of Galactic chemical evolution that ther-process isotopic abundance pattern can change as a function of cosmic time fordifferent time-varying contribution from supernova and neutron star mergerr-process.

16th Rußbach School on Nuclear... / Registrants Book Yuta Yamazaki


Dr. Azzurra Zucchini #32



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Institution: Department of Physics and Geology, University of Perugia, Italy

Abstract Submission

Write your title and abstract here: Title: History of a meteorite: from the origin tothe lab. First results about the Rock Star project. Abstract: In Nuclear Astrophysicsmeteorites and their chemical and isotopic composition are used as very precisebenchmarks for nucleosynthesis models and to tests the consequences of newmeasured reaction rate on the production or destruction of a certain nucleus. Toemploy meteorite samples for those scopes they have to be carefully analysed(often using techniques imported from experimental nuclear physics) andclassified. Indeed meteorites, which are solid pieces of meteroids, asteroids orcomets that are not completely consumed during their passage throw theatmosphere of a planet or a satellite, can be of very different types and might formin several phases of accretion of stellar/planetary system. Even if one of them isconsidered “falls” or “findings” depending whether the fall event was observed ornot, is very important since the time spent by a meteorite on Earth causeschemical modifications due to the interaction with the terrestrial environment(Weisberg et al. 2006). The classification of meteorites has been approached bymany scientists. The most recent meteorite classification was suggested byWeisberg et al. (2006) and it basically divides meteorites in three main groups: (i)chondrites, the undifferentiated meteorites, (ii) primitive achondrites, those thatsuffered just partial melting and (iii) achondrites, differentiated meteorites. Amongthe three main groups, several sub-groups have been individuated (Weisberg et al.2006). Chondrites are the most primitive meteorites available and containsdifferent components such as chondrules, Ca-Al rich inclusions (CAIs),(Fe,Ni)-metal, and a fine grained matrix. Moreover, sub-micrometric presolargrains (diamonds, silicon carbide, oxides, graphite, …) might be usually found. Themineralogical associations in chondrites meant that the material has not sufferedenough heating to melt (Scheinberg et al. 2015). On the contrary, differentiatedachondrites are meteorites originated from a differentiated parent body whereheating above the melting temperature of iron-nickel alloys allowed the migration ofthe heaviest elements toward the planetesimal core (source of iron meteorites) andthe migration of the lightest elements toward the crust (source of stonyachondrites). The differentiation process is believed to be occurred during the firstfew million years after the formation of CAIs (Scheinberg et al. 2015). The mainsupposed heating sources for planetesimal differentiation are (i) the radiogenicheating from short-lived radioisotopes 26Al and 60Fe (Moskovitz and Gaidos 2011;Scheinberg et al. 2015 and references therein), (ii) the gravitational energy ofaccretion and, less plausibly (iii) the electromagnetic induction heating (Scheinberget al. 2015 and references therein). The detailed analysis of the isotopiccomposition of meteorites is a fundamental contribution in order to give insight into

16th Rußbach School on Nuclear... / Registrants Book Azzurra Zucchini


processes and timing which ruled the primordial nucleosynthesis and the SolarSystem formation. The required multi-analytical approach joins different techniquessuch as Field-Emission Scanning Electron Microscopy, Raman analysis, X-rayPowder Diffraction, Electron-Probe Micro Analysis, Laser AblationInductively-Coupled-Plasma Mass Spectrometry and Secondary Ion MassSpectrometry. By means of these techniques the research group fullycharacterized different meteorite samples and gave important data to constrainabout the origin and evolution of planetesimal differentiation. Results obtained fromthe chemical, mineralogical and isotopic characterization of the Mineo pallasite(e.g. Zucchini et al. 2018) are presented. The Mineo meteorite belongs to the MainGroup pallasites. However, the olivines show peculiar features in terms of chemicalcomposition (e.g. iron from 9.1 to 11.5 wt%, positive correlation of Ca withcompatible elements such as Cr) and isotopic composition [δ(18O) from 2.06±0.02to 2.76±0.09]. The non-homogeneity of olivines within the same pallasite samplesuggests either a terrestrial chemical alteration or genetic processes wheredifferent portions of the Mineo pallasite likely comes from different areas of thesame differentiated parent body, and the residual molten Fe-Ni. Acknowledgments:The research group is acknowledged: Busso M., Comodi P., Frondini F., PalmeriniS. and Petrelli M. from the University of Perugia and INFN Perugia (Italy); CanteriR. and Pepponi G. from the Bruno Kessler Foundation (Trento, Italy); Di Leva A.,Di Rienzo B., Gialanella L., Marzaioli F. from the University of Campania (Italy).The project is supported by the ERNA project (INFN, Italy). References MoskovitsN., Gaidos E. (2011) Differentiation of planetesimals and the thermalconsequences of melt migration. MAPS, 46, 903 – 918. Scheinberg A., Fu R.R.,Elkins-Tanton L.T., Weiss B.P. (2015) Asteroid Differentiation: Melting andLarge-Scale Structure. Asteroids IV (P. Michel et al., eds.), Univ. of Arizona,Tucson, 533 – 552. Weisberg M.K., McCoy T.J., Krot A.N. (2006) Systematics andEvaluation of Meteorite Classification. Meteorites and the Early Solar System II(D.S. Lauretta and H.Y. McSween Jr. eds.), University of Arizona, Tucson, 19 – 52.Zucchini A., Petrelli M., Frondini F., Petrone C.M., Sassi P., Di Michele A.,Palmerini S., Trippella O., Busso M. (2018) Chemical and mineralogicalcharacterization of the mineo (Sicily, Italy) pallasite: A unique sample. MAPS, 53,268 – 283.

16th Rußbach School on Nuclear... / Registrants Book Azzurra Zucchini


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