Nuclear astrophysics experiments with stored highly

Tsukuba Global Science Week 2021International Workshop on "Universe Evolution and Matter Origin”

11 September 2021

Yuri A. Litvinov

Nuclear astrophysics experiments with stored highly-charged ions:

Latest experiments at GSI

Storage - efficient use of rare species

Cooling - high quality beams

Recirculation - high luminocities though thin targets

Removing of contaminants

Ultra-high vacuum – preserving atomic charge state

High detection efficiencies for recoils

Numerous dedicated detectors

Why storage rings? - Versatile Capabilities

Beam Accumulation

Large Acceptance

Beam Bunching

Beam Cooling:- Stochastic- Electron- (Laser)

Acceleration/Deceleration

UHV

Detection:- Electrons- Photons- Recoils

Various targets:- Electrons- Photons- Atoms- (Ions)- (Neutrons)

Internal Gas-Jet Target

Non-destructive particle detection

Physics at Storage Rings

ESR at GSI

CSRe at IMP

CRYRING at GSI

R3 at RIKEN

Storage rings stay for:Single-particle sensitivityBroad-band measurementsHigh atomic charge statesHigh resolving power

Photos: M. Lestinsky, A. Zschau, GSI; IMP Lanzhou; RIKEN

Where and how was gold cooked?

r - process

rp

- process

82

126

82

neutron number

50

288

28

20

20

8

pro

ton n

um

ber

s-process

NASA/Dana Berry

ESA, CC BY-SA 3.0 IGO

Hubble GalleryNASA, ESA, J. Hester, A. Loll

Hubble Gallery, NASA, ESA

ALMA (ESO/NAOJ/NRAO)

Hyosun Kim et al.

Where and how was gold cooked?

r - process

rp

- process

82

126

82

neutron number

50

288

28

20

20

8

pro

ton n

um

ber

s-process

masses determine the pathways of nucleosynthesisprocesses

β half-lives reflect the accumulated abundances

Rates of relevant reactions

Fragment Separator

FRS

Radioactive Ion Beam Facility at GSI

Productiontarget

StorageRingESR

Heavy-IonSynchrotron

SIS

LinearAccelerator

UNILAC

Picture: GSI, Darmstadt

Bound-State β-decay

Y. Litvinov & F. Bosch, Rep. Prog. Phys. 74, 016301 (2011)

Bound-State Beta Decay of 205Tl Nuclei

FAIR - Facility for Antiproton and

Ion Research in Europe GmbH

GSI Helmholtzzentrum für

Schwerionenforschung GmbH

Planckstrasse 1 64291 Darmstadt Germany

1 For any future reference please use this ID

Management Board, Geschäftsführung: Professor Dr. Paolo Giubellino Ursula Weyrich Jörg Blaurock

Chair of the Council/Supervisory Board, Vorsitzender des Aufsichtsrates: Staatssekretär Dr. Georg Schütte FAIR: Registered in, Sitz: Darmstadt Amtsgericht Darmstadt HRB 89372

VAT-ID: DE 275 595 927

Commerzbank Darmstadt IBAN DE03 5084 0005 0132 6305 00 BIC COBADEFF508

GSI: Registered in, Sitz: Darmstadt Amtsgericht Darmstadt HRB 1528

VAT-ID: DE 111 671 917

Landesbank Hessen/Thüringen IBAN DE56 5005 0000 5001 8650 04 BIC HELA DE FF

FAIR/GSI · Planckstr. 1 · 64291 Darmstadt · Germany Scientific Managing Director

Professor Dr. Paolo Giubellino Phone +49-6159-71-2649 [email protected]

11.10.2017

Yuri Litvinov

- GSI -

E121: “Measurement of the bound-state beta decay of bare 205

Tl

ions”

Yuri Litvinov et al.

Dear Colleague,

The management of GSI/FAIR would like to thank you for submitting a proposal to our latest ‘Call for Proposals for Beam Time in 2018/2019’. The General Program Advisory Committee met on September 19-21, 2017 (G-PAC43 meeting), to evaluate a total of 64 proposals requesting 2035 shifts of beam time. The considerations of the G-PAC were based on their assessment of the scientific importance of the proposed research, its feasibility and its reliance on aspects of the GSI/FAIR facility that are unique. Proposals were ranked into 4 categories with experiments of category A recommended to be done. Category A- experiments are of great scientific interest but due to the large overdraft of beam time can be recommended to run only if beam time becomes available (reserve list). Experiments of category B are those that are encouraged to submit an amended proposal to a future call, and for category C experiments no beam time is recommended. In total, the G-PAC recommended 816 shifts of category A, of which 311 shifts are at UNILAC, 317 shifts at SIS18, 122 shifts at ESR and 66 shifts at CRYRING. Shifts granted as experiments category A in this ‘Call’ will be scheduled between 2018 and 2019 and will expire after that period. For your proposal E1211 the G-PAC formulated the following evaluation with which I concur: Regarding the proposal “Measurement of the bound-state beta decay of bare

205Tl

ions” (Proposal E121), the G-PAC recommends this proposal with highest priority (A) and that 21 shifts of main beam time be allocated for this measurement.

Further Steps

� For scheduling your experiment, please contact your GSI contact person.

� The department “Safety and Radiation Protection” is to be informed on the planned set-up of the experiment and their consent is required before running an experiment. Your GSI contact person might help you with this

2

Proposal for an experiment to be conducted at FRS/ESR Measurement of the bound-state beta decay of bare 205Tl ions

Updated from previously accepted proposal E100

Fritz Bosch†, H. Geissel, J. Glorius, R. Grisenti, A. Gumberidze, S. Hagmann, Ch. Kozhuharov, M. Lestinsky, S. A. Litvinov, Yu. A. Litvinov, I. Mukha, C. Nociforo, F. Nolden, N. Petridis, R. Sánchez, M. S. Sanjari, C. Scheidenberger, U. Spillmann, M. Steck, T. Stöhlker, K. Takahashi, S. Trotsenko, H. Weick, N. Winckler, D. Winters GSI Helmholtzzentrum für Schwerionenforschung, 64291 Darmstadt, Germany C. Brandau I. Physik. Institut, Justus-Liebig Universität Giessen, 35392 Gießen, Germany R. Reifarth, Ch. Langer J.W. Goethe Universität, 60438 Frankfurt, Germany D. Atanasov, K. Blaum MPI für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany T. Faestermann, R. Gernhäuser, Paul Kienle‡, M. A. Najafi TU Munich, Phys. Depatment E12, D 85748 Garching, Germany M.K. Pavicevic Division of Material Sciences and Physics, Salzburg University, 5020 Salzburg, Austria W.F. Henning Physics Division, Argonne National Laboratory, Argonne, Illinois, USA Bradley S. Meyer, Department of Physics and Astronomy, Clemson University, SC-29634-0978, USA D. Schneider Lawrence Livermore National Laboratory, Livermore, CA 94551, USA K. G. Leach Department of Physics, Colorado School of Mines, CO-80401, Golden, USA V. Pejovic, Institute of Physics, Zemun, Pregrevica 118, 11000 Belgrade, Serbia B. Boev Faculty of Mining and Geology, University of Štip, 92000 Štip, FYR Macedonia T. Suzuki, T. Yamaguchi Saitama University, Saitama 338-8570, Japan S. Naimi, F. Suzaki, T. Uesaka, Y. Yamaguchi RIKEN Nishina Center, Wako, Tokyo, Japan T. Ohtsubo Department of Physics, Niigata University, Niigata 950-2181, Japan

† Deceased 16.12.2016 ‡ Deceased 29.01.2013

3

B. H. Sun School of Physics and Nuclear Energy Eng., Beihang University, Beijing 100191, China

X. C. Chen, B. S. Gao, X. W. Ma, X. L. Tu, M. Wang, H. S. Xu, X. L. Yan, Y. H. Zhang Institute of Modern Physics, Chinese Academy of Sciences, 730000 Lanzhou, China

C. Bruno, T. Davinson, C. Lederer-Woods, P. J. Woods School of Physics and Astronomy, University of Edinburgh, EH9 3JZ, UK

P. M. Walker Department of Physics, University of Surrey, Guildford, GU2 7XH, UK

G. Lane Department of Nuclear Physics, Research School of Physics and Engineering, The Australian National University, Canberra, ACT 2601, Australia I. Dillmann Nuclear Astrophysics Group, TRIUMF, Vancouver, British Columbia V6T2A3, Canada

M. Trassinelli Inst. des NanoSciences de Paris, CNRS UMR7588 and UMPC-Paris 6, 75015 Paris, France

S. Yu. Torilov St. Petersburg State University, St. Petersburg, Staryj Peterhof, Russian Federation

R. B. Cakirli, F. C. Ozturk Department of Physics, University of Istanbul, 34134 Istanbul, Turkey

B. Jurado CNRS, IN2P3, CENBG, UMR 5797, 33175 Gradignan, France

W. Korten IRFU, CEA, Université Paris-Saclay, 91191 Gif-sur-Yvette, France

For the LOREX, NucCAR, SPARC and ILIMA Collaborations

This project is in part supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 682841 “ASTRUm”)



NASA/SDO Termination of s-process

Fate of 205Pb in early Solar system

Detection of Solar pp-neutrinos

Solar Neutrino Flux

Courtesy R. J. Chen and R. Singh Sidhu

Lorandite TlAsS2 Mineral

LOREX Project

Age = 4.31(2) Ma

M. Pavicevic et al., NIM A895, 62 (2018)

December 2019

EMMI Rapid Reaction Task Force onThe LOREX Project



Experiment during the COVID1923.03 – 01.04 – 06.04

Enriched 206Pb beam

Separation from 205Pb81+

I(205Tl81+)/I(205Pb81+)= 1/15

Accumulation

Long breeding time

Separation of decaydaughter ions from

parent ions


Accumulation of 205Tl81+ beam in the ESR


Typical Measurement (5 Hours)


Icool = 20 mA

Icool = 200 mA

Ar-jet (10 min)

Electron cooler power failure

Preliminary Results


PHYSICAL REVIEW C 104, 024304 (2021)

Investigation of bound state β− decay half-lives of bare atoms

Shuo Liu, Chao Gao, and Chang Xu *

School of Physics, Nanjing University, Nanjing 210093, China

(Received 9 June 2021; accepted 21 July 2021; published 2 August 2021)

We investigate the bound state β− decay of highly ionized atoms, in which the decay electron remains in abound atomic state rather than being emitted into the continuum. A survey of 3344 nuclei is performed in orderto search possible bound state β− decay nuclei. We find that, for candidates 163Dy, 193Ir, 194Au, 202Tl, 205Tl, 215At,222Rn, 243Am, and 246Bk, the channel of β− decay is completely forbidden in the neutral case but can be openedin the bare case. The corresponding bound-state β− decay half-lives of these nuclei are predicted by using theTakahashi-Yokoi model, which are found to be significantly different from those in the neutral case.

DOI: 10.1103/PhysRevC.104.024304

I. INTRODUCTION

β− decay is one of the most important decay modes forunstable nuclei by converting a neutron to proton with anelectron and an antineutrino created in continuum states [1]. In1947, Daudel et al. first proposed the concept of bound-stateβ− decay and predicted that there might exist nuclear β−

decay accompanied with the electron created directly in an un-occupied atomic orbital [2]. For neutral atoms or moderatelyionized atoms, the bound-state β− decay with electron createdin the atomic orbital can hardly proceed. This is because onlyweakly bound states are available for the decay electron andthe bound state β− decay is only a marginal decay branch.However, for highly ionized atoms, more and more emptystates are available and the bound-state β− transition intodeeply bound orbits becomes possible [3]. For instance, withthe extremely high temperature and density, the atoms in thestellar plasma are partially or fully ionized and the bound-stateβ− decay is found to be important for both the pathways of nu-cleosynthesis and the abundances of the created nuclide [4,5].Therefore, the bound-state β− decay has attracted much atten-tion [6–11] and its first observation was successfully made for163Dy in 1992 [12]. The question of β− decay into the boundstates was investigated by Batkin in Ref. [13]. Takahashi et al.performed a detailed calculation on the β− decay rates forhighly ionized heavy atoms in a plasma of electrons and ionsat high temperature and high density [9]. It was found thatthe bound-state β− decay channel could lead to a significantchange in their total half-lives. For example, the 187Re hasan exceptionally long half-life (4.28 ± 0.08) × 1010 y in theneutral case, which is used to estimate the lower bound forthe age of our galaxy [14,15]. However, in the bare case thebound-state β− decay of 187Re to the first-excited state in187Os is opened and its total half-life is reduced dramaticallyfrom 4.28 × 1010 y to 32.9 y [16].

Previous research into bound-state β− decay mainly fo-cuses on atoms which are considered to be important for

*[email protected]

the slow neutron-capture process (s process) [10,11]. Thes process is responsible for the synthesis of approximatelyhalf the atomic nuclei heavier than iron via a sequence ofneutron captures and β− decays. For these atoms, the β−

decay process may occur in both the neutral and bare cases.Here we are interested in a special group of atoms, in whichthe channel of β− decay is totally forbidden in the neutralcase by the energy conservation law, but can be opened in thebare case. To the best of our knowledge, a systematic study onthese atoms is still missing. In present work, we perform a sur-vey of 3344 nuclei in the mass range 2 ! A ! 270 to searchfor atoms with possible β− decay channels in the condition ofcomplete ionization. It is found that only a few nuclei satisfythe required energy conditions, namely 163Dy, 193Ir, 194Au,202Tl, 205Tl, 215At, 222Rn, 243Am and 246Bk. In particular, thebound-state β− decays of 194Au, 202Tl, 215At, 222Rn, 243Am,and 246Bk have not yet been reported in previous works. Basedon the Takahashi-Yokoi model [9], the bound-state β− decayrates of these nuclei with electrons created in different atomiclow-lying states are predicted.

The paper is organized as follows: In Sec. II, we givethe energy criteria for selecting bound-state β− decaynuclei. The formulas of the Takahashi-Yokoi model for cal-culating the bound-state β− decay rates are also given. InSec. III, we discuss the estimated log f t values and the elec-tron radial wave functions in different atomic low-lying states.The calculated bound-state β− decay half-lives of suitablecandidates are given. Section IV gives a short summary.

II. METHODOLOGY

In the neutral case, the β− decay energy Qn is simply theenergy corresponding to the mass difference between parentand daughter atoms, and the experimental data of Qn can befound in Ref. [17]. For the bound-state β− decay in the barecase, the decay energy Qb is carried totally by the antineutrinoand can be defined as

Qb = Qn − [Bn(Z + 1) − Bn(Z )] + BK,L,..., (1)

2469-9985/2021/104(2)/024304(5) 024304-1 ©2021 American Physical Society

ATOMIC DATA AND NUCLEAR DATA TABLES 36,375-409 (1987)

BETA-DECAY RATES OF HIGHLY IONIZED HEAVY ATOMS IN STELLAR INTERIORS*

K. TAKAHASHI

University of California, Institute of Geophysics and Planetary Physics Lawrence Livermore National Laboratory, Livermore, California 94550

and

K. YOKOIt

Kernforschungszentrum Karlsruhe GmbH, Institut fur Kernphysik III D-7500 Karlsruhe, Federal Republic of Germany

Beta-decay rates are computed for heavy nuclides (26 < 2 Q 83, 59 i A < 210) at stellar temperatures of 5 X 10’ 4 T < 5 X 1 O8 K and electron number densities of 1 026 < n, < 3 X 1 O*’ cme3. The P-decay processes considered are: (i) electron emission (@- decay) into the continuum as well as into the bound state; (ii) positron emission (p’ decay); and (iii) capture of the orbital and free electrons. The degree of ionization is determined by solving the Saha equation corrected for the continuum depression within a finite-temperature Thomas-Fermi model. The adopted input atomic data are based on a self-consistent mean-field method. Theft values for unknown B transitions are estimated from systematics. The results will be most useful for s-process nucleosynthesis studies. o 1987 Academic PM, IX.

* Work performed in part under the auspices of the U.S. Department of Energy by the Lawrence Livermore National Laboratory under Contract W-740%Eng-48

t Present address: Science and Engineering Research Laboratory, Waseda University, Tokyo, Japan

0092-640X/87 $3.00 Copyright 0 1987 by Academic Press, Inc. All rights of reproduction in any form reserved. 375 Atomic Data and Nuclear Data Tables. Vol. 36. No. 3. May 1997

ATOMIC DATA AND NUCLEAR DATA TABLES 36,375-409 (1987)

BETA-DECAY RATES OF HIGHLY IONIZED HEAVY ATOMS IN STELLAR INTERIORS*

K. TAKAHASHI

University of California, Institute of Geophysics and Planetary Physics Lawrence Livermore National Laboratory, Livermore, California 94550

and

K. YOKOIt

Kernforschungszentrum Karlsruhe GmbH, Institut fur Kernphysik III D-7500 Karlsruhe, Federal Republic of Germany

Beta-decay rates are computed for heavy nuclides (26 < 2 Q 83, 59 i A < 210) at stellar temperatures of 5 X 10’ 4 T < 5 X 1 O8 K and electron number densities of 1 026 < n, < 3 X 1 O*’ cme3. The P-decay processes considered are: (i) electron emission (@- decay) into the continuum as well as into the bound state; (ii) positron emission (p’ decay); and (iii) capture of the orbital and free electrons. The degree of ionization is determined by solving the Saha equation corrected for the continuum depression within a finite-temperature Thomas-Fermi model. The adopted input atomic data are based on a self-consistent mean-field method. Theft values for unknown B transitions are estimated from systematics. The results will be most useful for s-process nucleosynthesis studies. o 1987 Academic PM, IX.

* Work performed in part under the auspices of the U.S. Department of Energy by the Lawrence Livermore National Laboratory under Contract W-740%Eng-48

t Present address: Science and Engineering Research Laboratory, Waseda University, Tokyo, Japan

0092-640X/87 $3.00 Copyright 0 1987 by Academic Press, Inc. All rights of reproduction in any form reserved. 375 Atomic Data and Nuclear Data Tables. Vol. 36. No. 3. May 1997

PHYSICAL REVIEW C 101, 031302(R) (2020)Rapid Communications

Calculated solar-neutrino capture rate for a radiochemical 205Tl-based solar-neutrino detector

Joel Kostensalo * and Jouni Suhonen †

University of Jyvaskyla, Department of Physics, P.O. Box 35, FI-40014, Finland

K. Zuber ‡

Institute for Nuclear and Particle Physics, TU Dresden, 01069 Dresden, Germany

(Received 19 December 2019; revised manuscript received 22 January 2020; accepted 19 February 2020;published 4 March 2020)

Radiochemical experiments for low-energy solar-neutrino detection have been making headlines by exploitingthe isotopes 37Cl and 71Ga. Such a very low-threshold measurement of this type can also be performed using205Tl, which has been considered for decades for this purpose. A unique feature of this detector nucleus is theintegration in the solar-neutrino flux over 106 of years owing to its long-living daughter 205Pb. In this RapidCommunication, we have calculated for the first time the cross section for the charged-current solar-neutrinoscattering off 205Tl. Taking into account the solar-model-predicted neutrino fluxes and the electron-neutrinosurvival probabilities, a solar-neutrino capture rate of 62.2 ± 8.6 solar-neutrio units is determined, a valuesignificantly smaller than in previous estimates.

DOI: 10.1103/PhysRevC.101.031302

Introduction. Neutrinos play a key role in several aspects ofastroparticles and nuclear physics [1]. From the astrophysicalpoint of view, solar neutrinos can be monitored in real-timemeasurements which allows to study neutrino properties,stellar structure, and evolution. To date, real-time monitoringof various neutrino chain reactions has been performed bythe super-Kamiokande, the Sudbury Neutrino Observatory,KamLAND, and especially Borexino. Borexino was able toperform a common global fit of all the observed reactions ofpp, pep, 7Be, and 8B in one detector [2].

An alternative method to the above-mentioned ones, usedby the first solar-neutrino experiments, are the radio-chemicalobservations. These experiments employ the charged-currentneutrino-nucleus scattering reaction,

νe + (A, Z ) → e− + (A, Z + 1) (1)

for solar-neutrino detection. This reaction has been used in thepioneering Homestake experiment using 37Cl as the detectormaterial [3], and, in this experiment, a deficit with respectto expectation was found. First measurements of the funda-mental pp neutrinos were based on 71Ga (GALLEX, GNO,and SAGE). Several other nuclides, with different reactionthresholds, have been considered for more refined overallspectral analyses [4]. A very interesting candidate of this typeis 205Tl, which has a very low threshold for solar neutrinos.

The 205Tl reaction. The dominant charged-currentneutrino-nucleus reaction under discussion is

205Tl(1/2+) + νe → 205Pb(1/2−) + e−, (2)

*[email protected]†[email protected]‡[email protected]

which feeds the first excited state of 205Pb at 2.33 keV andis of first-forbidden nonunique type [5]. Only a tiny portionof the feeding goes to the 5/2− ground state of 205Pb, thecorresponding transition being first-forbidden unique [5,6].According to the current atomic mass evaluation [7], the Qvalue is given by 50.6 ± 0.5 keV, which is so far the lowestthreshold among radiochemical approaches for solar-neutrinodetection. This results in a total threshold of about 53 keVfor the transition (2). Furthermore, a unique feature of thisreaction is the possibility for long-term monitoring of theaverage solar-neutrino flux and, hence, the mean solar lumi-nosity over the past 4.31 × 106 yr due to the long half-lifeof 1.73(7) × 107 yr of 205Pb [8]. Hence, such a measurementcould shed light on the long-term stability of the Sun and,therefore, on the stability of stars, in general [4].

The first studies of the Tl experiment were performedby Refs. [9–12] which later became the LOREX experiment[13,14]. Although several experimental aspects have alreadybeen addressed or have been worked on, the major remaininguncertainty is the cross section for this reaction. Hence, it isessential to get a reliable estimate of this cross section andthis Rapid Communication reports on the calculation of thisimportant quantity using current state-of-the-art techniques.

Calculation of the 205Tl cross section. The calculations forthe neutrino-nucleus cross section are based on the O’Connellet al. [15] and Donnelly and Peccei [16] method for thetreatment of semileptonic processes in nuclei. Details of theformalism as it is applied here can be found from Ref. [17]. Astreamlined version has also been given in the recent papers[18,19].

The nuclear-structure calculations were performed inthe shell-model framework using the shell-model codeNUSHELLX@MSU [20] with the Hamiltonian khhe [21] in

2469-9985/2020/101(3)/031302(4) 031302-1 ©2020 American Physical Society

Nuclear reaction studies in a storage ring

beam energy: 3 - 550 MeV/u ΔE/E: 10-4

rev. freq.: 250 kHz - 1 MHz H2 gas target: 1014 atoms/cm2

vacuum: 10-11mbar

ESRExperimental Storage Ring

Courtesy J. Glorius

High revolution frequency à high luminosity even with

thin targets

Detection of ions via in-ring particle detectors, clean beam and targetàlow background, high efficiency

Well-known atomic charge-exchange rates àin-situ luminosity monitor

in-flight fragmentation at FRSàapplicable to radioactive nuclei

Ultra-thin windowless gas targets and electron coolingà excellent energy resolution

deceleration of beamsàGamow window

very efficient use of exotic beams for high resolution experiments

Internal target

Proton-Capture Reactions in the ESR

ESR

gas jet

particledetectors

§ injection of ions @ >100 MeV/uü fully stripped ions

§ deceleration & cooling of the beamü E = 3 - 10 MeV/u

§ activate internal hydrogen targetü proton & electron capture reactionsü separated by dipole ü particle detectors on…

… inner tracks for (p,g) products… outer tracks for e- capture products

§ beam life time (residual gas + target interaction)Ø intensity goes down

dipole

electr

on

coole

r

refil

l rin

g pe

riodi

cally

Courtesy J. Glorius

Jan Glorius: “A recycling recoil separator”

In-Situ Luminosity Monitoring

gas jet

K-R

EC

L-R

ECM-R

EC Ka

Kb

X-ray spectrum @ 90°

total e- capture rate [NRC + REC]

radiative e- capture rate [REC]

measured by particle detection

X-ray spectroscopy

Courtesy J. Glorius

ESR

gas jet

124Xe(p,g)2nd generation detectors

50 m

m 16 x 16 strips

ceramic pcbU

HV c

ompa

tible

Courtesy J. Glorius

ESR Test Beam Time 2016 124Xe(p,g)125Cs

124Xe(p,g) - Results

6 MeV/u8 MeV/u7 MeV/u

x position y positi

on

6.7 MeV/u

x position y positi

on

5.5 MeV/u

Approaching the Gamow Window with Stored Ions:Direct Measurement of 124Xeðp;γÞ in the ESR Storage Ring

J. Glorius,1,* C. Langer,2 Z. Slavkovská,2 L. Bott,2 C. Brandau,1,3 B. Brückner,2 K. Blaum,4 X. Chen,5 S. Dababneh,6

T. Davinson,7 P. Erbacher,2 S. Fiebiger,2 T. Gaßner,1 K. Göbel,2 M. Groothuis,2 A. Gumberidze,1 G. Gyürky,8 M. Heil,1

R. Hess,1 R. Hensch,2 P. Hillmann,2 P.-M. Hillenbrand,1 O. Hinrichs,2 B. Jurado,9 T. Kausch,2 A. Khodaparast,1,2

T. Kisselbach,2 N. Klapper,2 C. Kozhuharov,1 D. Kurtulgil,2 G. Lane,10 C. Lederer-Woods,7 M. Lestinsky,1 S. Litvinov,1

Yu. A. Litvinov,1 B. Löher,11,1 F. Nolden,1 N. Petridis,1 U. Popp,1 T. Rauscher,12,13 M. Reed,10 R. Reifarth,2 M. S. Sanjari,1

D. Savran,1 H. Simon,1 U. Spillmann,1 M. Steck,1 T. Stöhlker,1,14 J. Stumm,2 A. Surzhykov,15,16 T. Szücs,8 T. T. Nguyen,2

A. Taremi Zadeh,2 B. Thomas,2 S. Yu. Torilov,17 H. Törnqvist,1,11 M. Träger,1 C. Trageser,1,3 S. Trotsenko,1 L. Varga,1

M. Volknandt,2 H. Weick,1 M. Weigand,2 C. Wolf,2 P. J. Woods,7 and Y. M. Xing5,11GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany

2Goethe Universität, Frankfurt am Main, Germany3Justus-Liebig Universität, Gießen, Germany

4Max-Planck-Institut für Kernphysik (MPIK), Heidelberg, Germany5Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou, China

6Al-Balqa Applied University, Salt, Jordan7University of Edinburgh, Edinburgh, United Kingdom

8Institute for Nuclear Research (MTA Atomki), Debrecen, Hungary9CENBG, CNRS-IN2P3, Gradignan, France

10Australian National University, Canberra, Australia11Technische Universität Darmstadt, Darmstadt, Germany12Department of Physics, University of Basel, Switzerland

13Centre for Astrophysics Research, University of Hertfordshire, Hatfield, United Kingdom14Helmholtz-Insitut Jena, Jena, Germany

15Physikalisch-Technische Bundesanstalt, Braunschweig, Germany16Technische Universität Braunschweig, Braunschweig, Germany

17St. Petersburg State University, St. Petersburg, Russia

(Received 6 December 2018; revised manuscript received 31 January 2019; published 7 March 2019)

We report the first measurement of low-energy proton-capture cross sections of 124Xe in a heavy-ionstorage ring. 124Xe54þ ions of five different beam energies between 5.5 and 8 AMeV were stored to collidewith a windowless hydrogen target. The 125Cs reaction products were directly detected. The interactionenergies are located on the high energy tail of the Gamow window for hot, explosive scenarios such assupernovae and x-ray binaries. The results serve as an important test of predicted astrophysical reactionrates in this mass range. Good agreement in the prediction of the astrophysically important proton width atlow energy is found, with only a 30% difference between measurement and theory. Larger deviations arefound above the neutron emission threshold, where also neutron and γ widths significantly impact the crosssections. The newly established experimental method is a very powerful tool to investigate nuclearreactions on rare ion beams at low center-of-mass energies.

DOI: 10.1103/PhysRevLett.122.092701

Charged-particle induced reactions like (p; γ) and(α; γ) and their reverse reactions play a central rolein the quantitative description of explosive scenarioslike supernovae [1] or x-ray binaries [2], where

temperatures above 1 GK can be reached. The energyinterval in which the reactions most likely occur underastrophysical conditions is called the Gamow window[3,4]. Experimentalists usually face two major chal-lenges when approaching the Gamow window: first, therelatively low center-of-mass energies of only a fewMeV or less, and second, the rapid decrease of crosssections with energy. The high stopping power con-nected to low-energy beams typically limits the amountof target material, and thus the achievable luminosity.

Published by the American Physical Society under the terms ofthe Creative Commons Attribution 4.0 International license.Further distribution of this work must maintain attribution tothe author(s) and the published article’s title, journal citation,and DOI.

PHYSICAL REVIEW LETTERS 122, 092701 (2019)

0031-9007=19=122(9)=092701(6) 092701-1 Published by the American Physical Society

J. Glorius, et al., PRL 122, 092701 (2019)

work of Laszlo Varga

Towards background free measurement

Courtesy J. Glorius and L. Varga

E127: Proton Capture on 118Te (05.2021)

Courtesy J. Glorius and L. Varga

study of radioactive 118Te (6 days half-life)production, storage, accumulation and deceleration of 118Te in FRS-ESRup to 1.000.000 118Te52+ ions stored proton-capture measurementsrealized at 7 MeV/u and 6 MeV/uclear signatures with good statistics

new background-free detection methodmaximized sensitivity for detection ofproton-capture reactions

future prospects:full access to Gamow window energies in CRYRING

124Xe(p,g)

118Te(p,g)

124Xe(p,g)

backgroundremoval

proton-capture

signature

7 MeV/u

The CRYRING@ESR facility

M. Lestinsky, GSI, DarmstadtM. Lestinsky et al., EPJ ST 225, 797 (2016)

CARME @ CRYRING(CRYRING Array for Reaction MEasurements)

Measure nuclear reactions directly at Big Bang energies

Novae physics

Reactions for p-process

Reactions for rp-process

Courtesy C. Bruno, T. Davinson, P. Woods

.....

Neutron-induced reactions(surrogate method)

B. Jurado, ERC AG „NECTAR“

FAIR - Facility for Antiproton and Ion Research

100 m

UNILACSIS 18

SIS 100/300

HESR

SuperFRS

NESR

CRRESR

GSI today Future facility

ESR

FLAIR

Ion Beam Facilities / Trapping & Storage

Stored and CooledHighly-Charged Ions (e.g. U92+) and Exotic Nuclei

From Rest to Relativistic Energies (up to 4.9 GeV/u)

Cooling: The Key for Precision

WorldwideUnique !

0,88 0,91 0,94 0,97 1,00 1,03 1,06 1,09 1,120,0

0,2

0,4

0,6

0,8

1,0

beam

inte

nsity

(arb

. unit

s)

f / f0

uncooled beam electron cooled beam

Dp/p ~ 10-5

0.95

0.87

0.77

0.44

0.67

0.80

0.62

0.57

0.52

0.48

0.40

inte

nsity

/ ar

b. u

nits

127300 127400 127500 127600 127700 127800 127900 128000 128100 128200

reco

rdin

g tim

e / s

econ

ds

0

30

60

90

120

150

180

240

192 81+Pb

192 81+Tl

frequency / Hz

e capture

Q = 3.37MeV

-

ec

From Single Ions to Highest Intensities

We are supported by:

Many thanks to our collaborators from all over the world !!!

Documents

Nuclear astrophysics experiments with stored highly