S1378: Lifetime Measurement of the MeV State in 23 Mg

Size: px
Start display at page:

Download "S1378: Lifetime Measurement of the MeV State in 23 Mg"

Transcription

1 S1378: Lifetime Measurement of the MeV State in 23 Mg Charles Akers, Peter Bender, Alison Cheeseman, Greg Christian, Randy Churchman, David Cross, Barry Davids, Lee Evitts, Jennifer Fallis, Naomi Galinski, Adam Garnsworthy, Greg Hackman, Steffen Ketelhut, Jonathan Lighthall, Oliver Kirsebom, Peter Machule, David Miller, Chantal Nobs, Chris Pearson, Allison Radich, Mustafa Rajabali, Alex Rojas, Alisher Sanetullaev, Carl Unsworth, Chris Ruiz, and Chris Wrede TRIUMF 21 Nov 2012

2 Classical novae periodicities range typically between yr). Both novae and supernovae are characterized by a remarkable energy output, with peak luminosities reaching 10 4 and L, respectively. A basic difference between both explosive phenomena is the amount of mass ejected (the whole star in a thermonuclear supernova versus M in a nova) as well as the mean ejection velocity (> 10 4 km s 1 in a supernova, and several 10 3 km s 1 in a classical nova). Z Model 1.35 M (50% ONe enrichment) T = K T ρ = g cm peak -3 ε nuc = erg g -1 s -1 ΔM env = M Si Al Mg Na C B Be Li He H O N Ne F N P S Ar Cl K Ca (p,γ) (p,α) (β + ) Log T = (Reaction 1 x Fluxes) 7 K : -2 : -3 : -4 : -5 : -6 : -7 Fig. 1. The main nuclear activity, shown in terms of reaction fluxes (number of reactions per unit volume J. José (2010) and time), at Tpeak, for a nova model of 1.35 M, with 50% ONe enrichment. The dominant nuclear reaction flow proceeds close to the valley of stability and is dominated by (p,γ), (p,α), and β-decays. See text for details.

3 1275 kev γ-ray line Na t 1/2 = 2.6 yr β kev γ Ne g.s.

4 Main destruction mechanism: 22 Na(p,γ) 23 Mg Two direct measurements both show that the reaction is dominated by a resonance at 206 kev (E x = 7786 kev, J π = 7/2 + ). But, the resonance strengths differ by a factor of 3: ωγ = 1.8 ± 0.7 mev Bochum [1] ωγ = mev Seattle [2] [1] Stegmüller et al., NPA 601, 168 (1996) [2] Sallaska et al., PRL 105, (2010); PRC 83, (2011)

5 Indirect determination of ωγ p 7/ kev kev 22 Na γ(7335 kev) γ(5734 kev) 7/2 + 5/2 + 3/ Mg 2052 kev 451 kev g.s. ωγ = 2J + 1 (2J a + 1)(2J A + 1) Γ p Γ γ Γ p + Γ γ

6 Indirect determination of ωγ Total width: Γ = Γ p + Γ γ Proton branching ratio: B p = Γ p /Γ Γ p Γ γ Γ p + Γ γ = B p (1 B p )Γ B p determined in recent 23 Al β-decay experiment [3], B p = ± Γ deduced from the lifetime, τ, determined in a recent 12 C( 12 C,n) 23 Mg experiment [4], using the doppler-shift attenuation method, τ = 10 ± 3 fs [3] Saastamoinen et al., PRC 83, (2011) [4] Jenkins et al., PRL 92, (2004)

7 Experimental situation ωγ = mev direct (Bochum) ωγ = mev direct (Seattle) ωγ = mev indirect

8 Doppler-shift attenuation method (DSAM) Principle: γ Previous experiment at TRIUMF ( 19 Ne) LIFETIMES OF STATES IN 19 Ne ABOVE THE... Mythili et al., PRC 77, (2008) 60 (a) γ Counts / 2.5 kev γ Energy (kev) τ = 1 fs 10 ps nts / 2.5 kev (b) τ = 7.1 ± 1.9 ± 0.6 fs

9 Experimental setup MeV Au 25 µm collimator 15 o ΔE 100 µm GRIFFIN Ge detector 3 He E 500 µm 3 He + 24 Mg α + 23 Mg E rel = 8.3 MeV, Q = 4.0 MeV 25 µm Au foil 3 He implantation depth = 0.1 µm, area density = cm 2 Clean γ-ray spectrum by gating on α particles.

10 Experimental setup

11 Run overview Net beam time = 4.8 days (74%) Av. FC0 = 1.6e10 pps (request 3.0e10 pps, min 0.6e10 pps) Av. R = 68.5 Ω ( 79.5 C) Av. P = 1.2e-7 torr scheduled beam time FC0, Event rate, P R FC0 [na] Event rate [per 0.1s] R [ohm] P [1e-8 torr] Nov 04 Nov 05 Nov 06 Nov 07 Nov 08 Nov 09 Nov 10 Nov 11 Nov 12 Nov 13 Nov 14 Nov

12 E-E plot ΔE (MeV) E (MeV)

13 Gate on 3 He loci Events / 2 kev t 1/2 =1.3 ps 24 Mg 1369 kev g.s. E γ (kev)

14 α-particle energy spectrum α 2 α 3 α 1 E+ΔE (MeV)

15 Known states in 23 Mg below 8 MeV

16 Known states in 23 Mg below 8 MeV α 3 α 2 α 1

17 Gate on all α particles Events / 2 kev 197 Au(279 gs) 23 Mg(451 gs) Au(548 gs) E γ (kev)

18 Gate on α 2 Events / 2 kev ₓ transition in 23 Mg ₓ not identified (yet) ₓ ₓ ₓ E γ (kev)

19 Gate on α 3 Events / 2 kev transition in 23 Mg E γ (kev)

20 Identified γ transitions between low-lying states in 23 Mg

21 23 Mg( ) transition E γ E γ (1 + v/c) 7335 kev ( ) = 7815 kev Solid angle δe γ ±7 kev Attenuation δe γ 9 kev (assuming τ = 10 fs) region of interest in gamma spectrum ( kev) background region ( kev) gamma counts δe gate (MeV)

22 23 Mg( ) transition signal 30 backgr 10 Events / 4 kev E γ (kev)

23 Summary The 1275 kev γ-ray line from 22 Na is considered the best known test of novae models Main destruction mechanism: 22 Na(p, γ) The two direct determinations of the 22 Na(p, γ) rate disagree A new measurement of the lifetime of the 7786 kev level is required to establish confidence in the indirect determination of the rate S1378: Attempt to determine lifetime using the DSAM method 75 MeV 24 Mg beam on 3 He implanted Au foil; coincident detection of α particles and γ rays at 0 Preliminary result: γ line observed, but statistics are not overwhelming

24 Doppler shift E γ = E γ (1 + β cos θ) In the limit t t slow down, β(t) Insert t = τ = 10 fs, M = 23 u, and (de/dx) t=0 = 8.0 MeV/µm a, t ( ) de Mc dx t=0 β(τ) Estimated variation in doppler shift: E γ E γ = MeV = 8.6 kev a stopping power of 45 MeV 23 Mg ions in Au

I. Gamma rays from novae

I. Gamma rays from novae A talk in two parts: I. Gamma rays from novae and II. New discoveries about the Hoyle state Oliver Kirsebom TRIUMF, Canada MSU, 11 March 2013 (JINA lunch-talk series) Part I. Gamma rays from novae S1378

More information

Doppler Shift Attenuation Method: The experimental setup at the MLL and the lifetime measurement of the 1 st excited state in 31 S

Doppler Shift Attenuation Method: The experimental setup at the MLL and the lifetime measurement of the 1 st excited state in 31 S Doppler Shift Attenuation Method: The experimental setup at the MLL and the lifetime measurement of the 1 st excited state in 31 S Clemens Herlitzius TU München (E12) Prof. Shawn Bishop Clemens Herlitzius,

More information

Explosive Events in the Universe and H-Burning

Explosive Events in the Universe and H-Burning Explosive Events in the Universe and H-Burning Jordi José Dept. Física i Enginyeria Nuclear, Univ. Politècnica de Catalunya (UPC), & Institut d Estudis Espacials de Catalunya (IEEC), Barcelona Nuclear

More information

Hydrogen and Helium Burning in Type I X-ray Bursts: Experimental Results and Future Prospects. Catherine M. Deibel Louisiana State University

Hydrogen and Helium Burning in Type I X-ray Bursts: Experimental Results and Future Prospects. Catherine M. Deibel Louisiana State University Hydrogen and Helium Burning in Type I X-ray Bursts: Experimental Results and Future Prospects Catherine M. Deibel Louisiana State University 8/29/14 CGS15 August 25 29, 2014 1 Click Type to I X-Ray edit

More information

Classical Novae at the Crossroads of Astrophysics, Nuclear Physics and Cosmochemistry

Classical Novae at the Crossroads of Astrophysics, Nuclear Physics and Cosmochemistry at the Crossroads of Astrophysics, Nuclear Physics and Cosmochemistry Jordi José Dept. Física i Enginyeria Nuclear, Univ. Politècnica de Catalunya (UPC) & Institut d Estudis Espacials de Catalunya (IEEC),

More information

Nuclear Astrophysics with DRAGON at ISAC:

Nuclear Astrophysics with DRAGON at ISAC: Nuclear Astrophysics with DRAGON at ISAC: The 21 Na(p, γ) 22 Mg reaction John M. D Auria for the DRAGON Collaboration Simon Fraser University Burnaby, British Columbia, Canada Abstract The DRAGON facility

More information

Precision measurements of. Na, 24 Al, 28 P, 32 Cl, and 36 K for the rp process

Precision measurements of. Na, 24 Al, 28 P, 32 Cl, and 36 K for the rp process Precision measurements of 20 Na, 24 Al, 28 P, 32 Cl, and 36 K for the rp process Chris Wrede Center for Experimental Nuclear Physics and Astrophysics University of Washington NIC XI, Heidelberg, Germany

More information

Presentation at the 10th RIBLL Collaboration Symposium, Beijing, 2017/1/7

Presentation at the 10th RIBLL Collaboration Symposium, Beijing, 2017/1/7 Presentation at the 10th RIBLL Collaboration Symposium, Beijing, 2017/1/7 Outline 1. Background 1.1 Decay for proton-rich nuclei 1.2 Astrophysical implications 2. Experiments 2.1 Introduction 2.2 Experimental

More information

The 33 S(p,γ) 34 Cl reaction in classical nova explosions

The 33 S(p,γ) 34 Cl reaction in classical nova explosions The 33 S(p,γ) 34 Cl reaction in classical nova explosions Anuj Parikh Physik Department E12 TU-München Galactic 26g Al (t 1/2 = 717 000 y) Galactic 34m Cl (t 1/2 = 32 min) N. Machiavelli et al. (R. Diehl

More information

Experimental Approach to Explosive Hydrogen Burning with Low-Energy RI Beams

Experimental Approach to Explosive Hydrogen Burning with Low-Energy RI Beams Hirschegg 06-1 Experimental Approach to Explosive Hydrogen Burning with Low-Energy RI Beams S. Kubono Center for Nuclear Study (CNS) University of Tokyo 1. Low Energy RI Beam Production 2. Proton Resonance

More information

Reaction rates in the Laboratory

Reaction rates in the Laboratory Reaction rates in the Laboratory Example I: 14 N(p,γ) 15 O slowest reaction in the CNO cycle Controls duration of hydrogen burning Determines main sequence turnoff glob. cluster ages stable target can

More information

IRIS Experiments S1396 and S1203

IRIS Experiments S1396 and S1203 Experiments S1396 and S1203 St. Mary s University/TRIUMF ISAC Science Forum Auditorium, TRIUMF November 2013, 2013 Outline Motivation Overview of Facility Experiment S1396 Experiment S1203 Summary Motivation

More information

DEFORMED STRUCTURES AND SHAPE COEXISTENCE IN 98 ZR

DEFORMED STRUCTURES AND SHAPE COEXISTENCE IN 98 ZR DEFORMED STRUCTURES AND SHAPE COEXISTENCE IN 98 ZR Bruno Olaizola University of Guelph, ON, Canada TRIUMF INPC2016 Adelaide, Australia 12 September 2016 Overview Shape coexistence in Zr isotopes High-statistics

More information

Going beyond the traditional nuclear shell model with the study of neutron-rich (radioactive) light nuclei

Going beyond the traditional nuclear shell model with the study of neutron-rich (radioactive) light nuclei Going beyond the traditional nuclear shell model with the study of neutron-rich (radioactive) light nuclei Fred SARAZIN Colorado School of Mines SORRY Overview What is low-energy nuclear physics? Stable

More information

Experimental Nuclear Astrophysics: Lecture 3. Chris Wrede National Nuclear Physics Summer School June 20 th, 2018

Experimental Nuclear Astrophysics: Lecture 3. Chris Wrede National Nuclear Physics Summer School June 20 th, 2018 : Lecture 3 Chris Wrede National Nuclear Physics Summer School June 20 th, 2018 Outline Lecture 1: Introduction & charged-particle reactions Lecture 2: Neutron-induced reactions Lecture 3: What I do (indirect

More information

Novae Reaction Rates and Measurements

Novae Reaction Rates and Measurements Nova Cygni Nova T Pyxidis Novae Reaction Rates and Measurements Measuring Nuclear Reaction Rates One Step at a Time Shawn Bishop, TUM Erice School, 2010 1 Talk Outline Astrophysics Primer Experimental

More information

Nuclear Astrophysics II

Nuclear Astrophysics II Nuclear Astrophysics II Lecture 5 Fri. June 1, 2012 Prof. Shawn Bishop, Office 2013, Ex. 12437 shawn.bishop@ph.tum.de http://www.nucastro.ph.tum.de/ 1 Where to from here? We are now at a crossroads for

More information

H/He burning reactions on unstable nuclei for Nuclear Astrophysics

H/He burning reactions on unstable nuclei for Nuclear Astrophysics H/He burning reactions on unstable nuclei for Nuclear Astrophysics PJ Woods University of Edinburgh H T O F E E U D N I I N V E B R U S I R T Y H G Explosive H/He burning in Binary Stars Isaac Newton,

More information

Neutron induced reactions & nuclear cosmo-chronology. chronology. A Mengoni IAEA Vienna/CERN, Geneva

Neutron induced reactions & nuclear cosmo-chronology. chronology. A Mengoni IAEA Vienna/CERN, Geneva Neutron induced reactions & nuclear cosmo-chronology chronology A Mengoni IAEA Vienna/CERN, Geneva Ages Cosmological way based on the Hubble time definition ( expansion age ) Astronomical way based on

More information

Determining Two Reaction Rates in Novae using the ANCs Technique. Tariq Al-Abdullah Hashemite University, Jordan Russbach, March 2011

Determining Two Reaction Rates in Novae using the ANCs Technique. Tariq Al-Abdullah Hashemite University, Jordan Russbach, March 2011 Determining Two Reaction Rates in Novae using the ANCs Technique Tariq Al-Abdullah Hashemite University, Jordan Russbach, March 2011 Main Points Synthesis of 22Na and 18F in ONe novae. Asymptotic Normalization

More information

Experimental Study of Stellar Reactions at CNS

Experimental Study of Stellar Reactions at CNS Experimental Study of Stellar Reactions at CNS Shigeru KUBONO ( 久保野茂 ) Center for Nuclear Study (CNS) University of Tokyo 1. Nucleosynthesis under Explosive Conditions + CNS-RIKEN AVF-Upgrade Project 2.

More information

A New Measurement of the E1 Component of

A New Measurement of the E1 Component of A New Measurement of the E1 Component of the 12 C(α,γ) 16 O Reaction X. Tang Physics Division Argonne National Laboratory Outline Why is the 12 C(α, γ) 16 O reaction important? The 12 C(α,γ) 16 O reaction

More information

High-resolution study of Gamow- Teller transitions in pf-shell nuclei. Tatsuya ADACHI

High-resolution study of Gamow- Teller transitions in pf-shell nuclei. Tatsuya ADACHI High-resolution study of Gamow- Teller transitions in pf-shell nuclei Tatsuya ADACHI Type II supernova Electron Capture (EC) & β decay Neutrino induced reaction A Z-1X N+1 daughter EC β A ZX N parent (A,Z)

More information

Department of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996, USA

Department of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996, USA Spin assignments of 22 Mg states through a 24 Mg(p,t) 22 Mg measurement, K. L. Jones, B. H. Moazen, S. T. Pittman Department of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996,

More information

Joint ICTP-IAEA Workshop on Nuclear Structure Decay Data: Theory and Evaluation August Experimental Nuclear Physics: Part 2

Joint ICTP-IAEA Workshop on Nuclear Structure Decay Data: Theory and Evaluation August Experimental Nuclear Physics: Part 2 2358-11 Joint ICTP-IAEA Workshop on Nuclear Structure Decay Data: Theory and Evaluation 6-17 August 2012 Experimental Nuclear Physics: Part 2 E. Ricard McCutchan Brookhaven National Lab. USA Experimental

More information

Research at FSU, using RESOLUT facility Development of and research with two new detector-systems

Research at FSU, using RESOLUT facility Development of and research with two new detector-systems Nuclear Astrophysics and Structure Research with Radioactive Beams Research at FSU, using RESOLUT facility Development of and research with two new detector-systems ResoNeut: Low-energy neutron detector-array

More information

Structure of neutron-rich Mg isotopes explored by beta-decay of spin-polarized Na isotopes

Structure of neutron-rich Mg isotopes explored by beta-decay of spin-polarized Na isotopes Structure of neutron-rich Mg isotopes explored by beta-decay of spin-polarized Na isotopes K. Tajiri, T. Shimoda, K. Kura, M. Kazato, M. Suga, A. Takashima, T. Masue, T. Hori, T. Suzuki, T. Fukuchi, A.

More information

Gamma-ray nucleosynthesis. Predictions - Gamma-ray nuclei - Production sites Observations - Point sources - Diffuse emission

Gamma-ray nucleosynthesis. Predictions - Gamma-ray nuclei - Production sites Observations - Point sources - Diffuse emission Gamma-ray nucleosynthesis N. Mowlavi Geneva Observatory Predictions - Gamma-ray nuclei - Production sites Observations - Point sources - Diffuse emission 1 I. Predictions 2 300 250 200 150 100 50 10 6

More information

Constraining Astrophysical Reaction Rates with Transfer Reactions at Low and Intermediate Energies

Constraining Astrophysical Reaction Rates with Transfer Reactions at Low and Intermediate Energies Constraining Astrophysical Reaction Rates with Transfer Reactions at Low and Intermediate Energies Christoph Langer (JINA/NSCL) INT Workshop: Reactions and Structure of Exotic Nuclei March 2015 1 Understanding

More information

Experimental Nuclear Astrophysics: Lecture 1. Chris Wrede National Nuclear Physics Summer School June 19 th, 2018

Experimental Nuclear Astrophysics: Lecture 1. Chris Wrede National Nuclear Physics Summer School June 19 th, 2018 : Lecture 1 Chris Wrede National Nuclear Physics Summer School June 19 th, 2018 Outline Lecture 1: Introduction & charged-particle reactions Lecture 2: Neutron-capture reactions Lecture 3: What I do (indirect

More information

Fast-Timing with LaBr 3 :Ce Detectors and the Half-life of the I π = 4 Intruder State in 34 P

Fast-Timing with LaBr 3 :Ce Detectors and the Half-life of the I π = 4 Intruder State in 34 P Fast-Timing with LaBr 3 :Ce Detectors and the Half-life of the I π = 4 Intruder State in 34 P P.J.R. Mason University of Surrey Seminar, 11th October 2011 Outline Characteristics of LaBr 3 detectors Fast-timing

More information

Stellar Evolution: what do we know?

Stellar Evolution: what do we know? Stellar Evolution: what do we know? New Tools - Astronomy satellite based observatories Hubble Space Telescope Compton Gamma-Ray Observatory Chandra X-Ray Observatory INTEGRAL ground based observatories

More information

Supernova events and neutron stars

Supernova events and neutron stars Supernova events and neutron stars So far, we have followed stellar evolution up to the formation of a C-rich core. For massive stars ( M initial > 8 M Sun ), the contracting He core proceeds smoothly

More information

Measurements for 44 Ti at TRIUMF-ISAC 40

Measurements for 44 Ti at TRIUMF-ISAC 40 Measurements for Ti at TRIUMF-ISAC 40 Ca(, ) Ti and future RIB experiments (ETH Zurich) for the DRAGON collaboration Vancouver, B.C., Canada Role of Ti in Astrophysics laboratory half-life of 58.9 +/-

More information

Decay spectroscopy for nuclear astrophysics

Decay spectroscopy for nuclear astrophysics Decay spectroscopy for nuclear astrophysics 1 Cyclotron Institute, Texas A&M University College Station, TX 77843-3366, USA E-mail: livius_trache@tamu.edu Abstract. In many radiative proton capture reactions

More information

Resonant Reactions direct reactions:

Resonant Reactions direct reactions: Resonant Reactions The energy range that could be populated in the compound nucleus by capture of the incoming projectile by the target nucleus is for direct reactions: for neutron induced reactions: roughly

More information

Inelastic Neutron Scattering Studies: Relevance to Neutrinoless Double-β Decay. Steven W. Yates

Inelastic Neutron Scattering Studies: Relevance to Neutrinoless Double-β Decay. Steven W. Yates Inelastic Neutron Scattering Studies: Relevance to Neutrinoless Double-β Decay Steven W. Yates TRIUMF Double-β Decay Workshop 13 May 2016 Questions What experimental data should theory reproduce so we

More information

Sunday Monday Thursday. Friday

Sunday Monday Thursday. Friday Nuclear Structure III experiment Sunday Monday Thursday Low-lying excited states Collectivity and the single-particle degrees of freedom Collectivity studied in Coulomb excitation Direct reactions to study

More information

Nuclear Astrophysics at the ISAC Radioactive Beams Facility: Prelude for RIA

Nuclear Astrophysics at the ISAC Radioactive Beams Facility: Prelude for RIA Nuclear Astrophysics at the ISAC Radioactive Beams Facility: Prelude for RIA John D Auria for the DRAGON Collaboration Radioachemistry at RIA Symposium 225 th National ACS Meeting, New Orleans March 27,

More information

Addendum to the ISOLDE and Neutron Time-of-Flight Committee

Addendum to the ISOLDE and Neutron Time-of-Flight Committee ` EUROPEAN ORGANIZATION FOR NUCLEAR RESEARCH Addendum to the ISOLDE and Neutron Time-of-Flight Committee IS530: Properties of low-lying intruder states in 34 Al and 34 Si sequentially populated in beta-decay

More information

Nuclear Astrophysics - I

Nuclear Astrophysics - I Nuclear Astrophysics - I Carl Brune Ohio University, Athens Ohio Exotic Beam Summer School 2016 July 20, 2016 Astrophysics and Cosmology Observations Underlying Physics Electromagnetic Spectrum: radio,

More information

DEVELOPMENT OF A NEW POSITRON LIFETIME SPECTROSCOPY TECHNIQUE FOR DEFECT CHARACTERIZATION IN THICK MATERIALS

DEVELOPMENT OF A NEW POSITRON LIFETIME SPECTROSCOPY TECHNIQUE FOR DEFECT CHARACTERIZATION IN THICK MATERIALS Copyright JCPDS - International Centre for Diffraction Data 2004, Advances in X-ray Analysis, Volume 47. 59 DEVELOPMENT OF A NEW POSITRON LIFETIME SPECTROSCOPY TECHNIQUE FOR DEFECT CHARACTERIZATION IN

More information

MAJOR NUCLEAR BURNING STAGES

MAJOR NUCLEAR BURNING STAGES MAJOR NUCLEAR BURNING STAGES The Coulomb barrier is higher for heavier nuclei with high charge: The first reactions to occur are those involving light nuclei -- Starting from hydrogen burning, helium burning

More information

FAST-TIMING CAPABILITIES OF GRIFFIN

FAST-TIMING CAPABILITIES OF GRIFFIN FAST-TIMING CAPABILITIES OF GRIFFIN Bruno Olaizola for the GRIFFIN collaboration University of Guelph, ON, Canada TRIUMF Nu-ball workshop, Orsay, France 19 May 2016 TRIUMF GRIFFIN Fast timing Future plans

More information

Carbon Burning in the Universe and the Laboratory

Carbon Burning in the Universe and the Laboratory Carbon Burning in the Universe and the Laboratory X. Tang University of Notre Dame Carbon burning processes in the Universe Carbon burning in the laboratory Limits on the molecular resonance strengths

More information

SURROGATE REACTIONS. An overview of papers by Jason Burke from LLNL

SURROGATE REACTIONS. An overview of papers by Jason Burke from LLNL SURROGATE REACTIONS An overview of papers by Jason Burke from LLNL Compound Nuclear Reaction cross sections Cross sections for compound-nuclear reactions are required input for astrophysical models and

More information

Decay Spectroscopy Experiments with GRIFFIN at ISAC- TRIUMF

Decay Spectroscopy Experiments with GRIFFIN at ISAC- TRIUMF SIMON FRASER UNIVERSITY ENGAGING THE WORLD Decay Spectroscopy Experiments with GRIFFIN at ISAC- TRIUMF Corina Andreoiu Department of Chemistry Simon Fraser University Burnaby, BC, Canada SSNET 2017 Paris,

More information

in2p , version 1-28 Nov 2008

in2p , version 1-28 Nov 2008 Author manuscript, published in "Japanese French Symposium - New paradigms in Nuclear Physics, Paris : France (28)" DOI : 1.1142/S21831391444 November 23, 28 21:1 WSPC/INSTRUCTION FILE oliveira International

More information

Absolute Determination of the 22 Na(p, γ) 23 Mg Reaction Rate: Consequences for Nucleosynthesis of 22 Na in Novae

Absolute Determination of the 22 Na(p, γ) 23 Mg Reaction Rate: Consequences for Nucleosynthesis of 22 Na in Novae Absolute Determination of the 22 Na(p, γ) 23 Mg Reaction Rate: Consequences for Nucleosynthesis of 22 Na in Novae Anne L. Sallaska A dissertation submitted in partial fulfillment of the requirements for

More information

Application of positrons in materials research

Application of positrons in materials research Application of positrons in materials research Trapping of positrons at vacancy defects Using positrons, one can get defect information. R. Krause-Rehberg and H. S. Leipner, Positron annihilation in Semiconductors,

More information

Positron Annihilation in Material Research

Positron Annihilation in Material Research Positron Annihilation in Material Research Introduction Positron sources, positron beams Interaction of positrons with matter Annihilation channels: Emission of 1, 2 or 3 γ-quanta Annihilation spectroscopies:

More information

Lecture #1: Nuclear and Thermonuclear Reactions. Prof. Christian Iliadis

Lecture #1: Nuclear and Thermonuclear Reactions. Prof. Christian Iliadis Lecture #1: Nuclear and Thermonuclear Reactions Prof. Christian Iliadis Nuclear Reactions Definition of cross section: = N r N 0 N t Unit: 1 barn=10-28 m 2 Example: 1 H + 1 H 2 H + e + + ν (first step

More information

Ness LUNA II facility. INFN underground Gran Sasso Laboratories. P. Corvisiero INFN - Italy

Ness LUNA II facility. INFN underground Gran Sasso Laboratories. P. Corvisiero INFN - Italy Ness 2002 LUNA II facility INFN underground Gran Sasso Laboratories P. Corvisiero INFN - Italy the pp chain p + p d + e + + + ν e e d + p 3 3 He He + γγ 84.7 % 13.8 % 3 3 He He + 3 3 He He α + 2p 3 2p

More information

at Gran Sasso Laboratories, Italy

at Gran Sasso Laboratories, Italy Underground Nuclear Astrophysics at Gran Sasso Laboratories, Italy Francesca Cavanna Università di Genova and INFN Genova, Italy Helmholtz Zentrum Dresden Rossendorf, Germany Laboratory Underground Nuclear

More information

LECTURE 6: INTERACTION OF RADIATION WITH MATTER

LECTURE 6: INTERACTION OF RADIATION WITH MATTER LCTUR 6: INTRACTION OF RADIATION WITH MATTR All radiation is detected through its interaction with matter! INTRODUCTION: What happens when radiation passes through matter? Interlude The concept of cross-section

More information

APPLICATION OF THE NUCLEAR REACTION ANALYSIS FOR AGING INVESTIGATIONS

APPLICATION OF THE NUCLEAR REACTION ANALYSIS FOR AGING INVESTIGATIONS 1 APPLICATION OF THE NUCLEAR REACTION ANALYSIS FOR AGING INVESTIGATIONS G.Gavrilov, A.Krivchitch, V.Lebedev PETERSBURG NUCLEAR PHYSICS INSTITUTE E-mail: lebedev@pnpi.spb.ru kriv@rec03.pnpi.spb.ru We used

More information

New Measurements of ψ(3770) Resonance Parameters & DD-bar Cross Section at BES-II & CLEO-c

New Measurements of ψ(3770) Resonance Parameters & DD-bar Cross Section at BES-II & CLEO-c New Measurements of ψ(3770) Resonance Parameters & DD-bar Cross Section at BES-II & CLEO-c The review talk is based on the talks given at ICHEP 04 by Anders Ryd, Ian Shipsey, Gang Rong 1 Outline Introduction

More information

Experimental Initiatives in Nuclear Astrophysics

Experimental Initiatives in Nuclear Astrophysics Experimental Initiatives in Nuclear Astrophysics Carl Brune Astrophysics: H and He burning, S process Facilities: neutron and gamma beams, underground accelerators, ICF plasmas Joint DNP Town Meetings

More information

Basics and Means of Positron Annihilation

Basics and Means of Positron Annihilation Basics and Means of Positron Annihilation Positron history Means of positron annihilation positron lifetime spectroscopy angular correlation Doppler-broadening spectroscopy Near-surface positron experiments:

More information

PoS(ENAS 6)050. Resonances in 19 Ne with relevance to the astrophysically important 18 F(p,α) 15 O reaction

PoS(ENAS 6)050. Resonances in 19 Ne with relevance to the astrophysically important 18 F(p,α) 15 O reaction Resonances in 19 Ne with relevance to the astrophysically important 18 F(p,α) 15 O reaction David Mountford, A.St J. Murphy, T. Davinson, P.J. Woods University of Edinburgh E-mail: d.j.mountford@sms.ed.ac.uk

More information

Ne(p,γ) 23 Na MEASUREMENT AT LUNA II AND IMPACT ON ASTROPHYSICAL SCENARIOS. MARIE-LUISE MENZEL for the LUNA collaboration

Ne(p,γ) 23 Na MEASUREMENT AT LUNA II AND IMPACT ON ASTROPHYSICAL SCENARIOS. MARIE-LUISE MENZEL for the LUNA collaboration 22 Ne(p,γ) 23 Na MEASUREMENT AT LUNA II AND IMPACT ON ASTROPHYSICAL SCENARIOS MARIE-LUISE MENZEL for the LUNA collaboration 1. INTRODUCTION 1.1 NEON-SODIUM-CYCLE 1.2 THE 22 Ne(p,γ) 23 Na REACTION INTRODUCTION

More information

Type II Supernovae Overwhelming observational evidence that Type II supernovae are associated with the endpoints of massive stars: Association with

Type II Supernovae Overwhelming observational evidence that Type II supernovae are associated with the endpoints of massive stars: Association with Type II Supernovae Overwhelming observational evidence that Type II supernovae are associated with the endpoints of massive stars: Association with spiral arms in spiral galaxies Supernova in M75 Type

More information

Measurementof 7 Be(n,α) and 7 Be(n,p) cross sections for the Cosmological Li problem in

Measurementof 7 Be(n,α) and 7 Be(n,p) cross sections for the Cosmological Li problem in Measurementof Be(n,α) and Be(n,p) cross sections for the Cosmological Li problem in EAR2@n_TOF M. Barbagallo, A. Musumarra, L. Cosentino, N. Colonna, P. Finocchiaro, A. Pappalardo and the n_tof Collaboration

More information

STUDY OF THE RESONANCES AT 417, 611, AND

STUDY OF THE RESONANCES AT 417, 611, AND STUDY OF THE RESONANCES AT 417, 611, AND 63 kev IN THE Ne(p,γ) 3 Na REACTION,a,b, Francesca Cavanna a,b, Rosanna Depalo c,d, Alessandra Slemer c,d, Tariq Al-Abdullah e,g, Michael Anders e, f, Daniel Bemmerer

More information

Se rp-process waiting point and the 69

Se rp-process waiting point and the 69 68 Se rp-process waiting point and the Kr -delayed proton emission experiment Marcelo Del Santo Joint Institute for Nuclear Astrophysics National Superconducting Cyclotron Laboratory Frontiers 2010 Workshop

More information

Lecture notes 8: Nuclear reactions in solar/stellar interiors

Lecture notes 8: Nuclear reactions in solar/stellar interiors Lecture notes 8: Nuclear reactions in solar/stellar interiors Atomic Nuclei We will henceforth often write protons 1 1p as 1 1H to underline that hydrogen, deuterium and tritium are chemically similar.

More information

The LUNA - MV project at the Gran Sasso Laboratory

The LUNA - MV project at the Gran Sasso Laboratory The LUNA - MV project at the Gran Sasso Laboratory Roberto Menegazzo for the LUNA Collaboration 3ème Andromède Workshop - Orsay, 9 Juillet 2014 outlook LUNA: Why going underground to measure nuclear fusion

More information

Physik-Department Institut für Experimentalphysik E12

Physik-Department Institut für Experimentalphysik E12 Physik-Department Institut für Experimentalphysik E12 The Doppler Shift Attenuation Method Facility: Its Design, Setup and Commissioning with the 32 S( 3 He, 4 He) 31 S Reaction Dissertation von Clemens

More information

Positron Annihilation Spectroscopy - A non-destructive method for material testing -

Positron Annihilation Spectroscopy - A non-destructive method for material testing - Maik Butterling Institute of Radiation Physics http://www.hzdr.de Positron Annihilation Spectroscopy - A non-destructive method for material testing - Maik Butterling Positron Annihilation Spectroscopy

More information

Oliver S. Kirsebom. Debrecen, 27 Oct 2012

Oliver S. Kirsebom. Debrecen, 27 Oct 2012 12 C and the triple-α reaction rate Oliver S. Kirsebom Debrecen, 27 Oct 2012 Aarhus University, Denmark & TRIUMF, Canada Introduction Astrophysical helium burning Red giant stars, T = 0.1 2 GK Three reactions:

More information

Radiative Capture Reaction

Radiative Capture Reaction A New Decay Path in the C+16O Radiative Capture Reaction Institut Pluridisciplinaire Hubert Curien, Strasbourg, France Outline Narrow Resonances, C +16O Detailed study of the C(16O,γ)28Si resonant radiative

More information

Reaction measurements on and with radioactive isotopes for nuclear astrophysics

Reaction measurements on and with radioactive isotopes for nuclear astrophysics Reaction measurements on and with radioactive isotopes for nuclear astrophysics René Reifarth GSI Darmstadt/University of Frankfurt NUCL Symposium: Radiochemistry at the Facility for Rare Isotope Beams

More information

DIPOLE-STRENGTH IN N=50 NUCLEI STUDIED IN PHOTON-SCATTERING EXPERIMENTS AT ELBE

DIPOLE-STRENGTH IN N=50 NUCLEI STUDIED IN PHOTON-SCATTERING EXPERIMENTS AT ELBE DIPOLE-STRENGTH IN N=50 NUCLEI STUDIED IN PHOTON-SCATTERING EXPERIMENTS AT ELBE R.Schwengner 1, G.Rusev 1, N.Benouaret 1,2, R.Beyer 1, F.Dönau 1, M.Erhard 1, E.Grosse 1,3, A.R.Junghans 1, K.Kosev 1, J.Klug

More information

Charge Exchange and Weak Strength for Astrophysics

Charge Exchange and Weak Strength for Astrophysics Charge Exchange and Weak Strength for Astrophysics Sam Austin STANfest-July 16 2004 Charge Exchange and Weak Strength for Astrophysics Interesting phenomena Electron capture strength (GT) (Langanke talk)

More information

Testing the validity of the Spin-orbit force Nuclear forces at the drip-line O. Sorlin (GANIL, Caen, France) PART 1:

Testing the validity of the Spin-orbit force Nuclear forces at the drip-line O. Sorlin (GANIL, Caen, France) PART 1: Testing the validity of the Spin-orbit force Nuclear forces at the drip-line O. Sorlin (GANIL, Caen, France) PART : The 34 Si a bubble nucleus? Probing the neutron SO interaction using the 34 Si nucleus

More information

Dipole resonances in 4 He

Dipole resonances in 4 He Dipole resonances in He σ( 7 Li, 7 Be), σ(ν,ν ), and σ γ S. Nakayama (Univ of Tokushima) Neutrino-induced reactions (neutral current) He(ν,ν ) in SN ν-heating He( 7 Li, 7 Be) Application of the He( 7 Li,

More information

Search for 24 Mg resonances inside the Gamowwindow for 12 C+ 12 Cfusion. Neven Soić, Ruđer Bošković Institute, Zagreb, Croatia

Search for 24 Mg resonances inside the Gamowwindow for 12 C+ 12 Cfusion. Neven Soić, Ruđer Bošković Institute, Zagreb, Croatia Search for 24 Mg resonances inside the Gamowwindow for C+ Cfusion C γ 24 Mg C γ Neven Soić, Ruđer Bošković Institute, Zagreb, Croatia Collaborators 1) S. Blagus, L. Grassi, D. Jelavić Malenica, T. Mijatović,

More information

Arjan Plompen. Measurements of sodium inelastic scattering and deuterium elastic scattering

Arjan Plompen. Measurements of sodium inelastic scattering and deuterium elastic scattering Arjan Plompen Measurements of sodium inelastic scattering and deuterium elastic scattering Overview Na inelastic scattering with GAINS C. Rouki et al., Nucl. Instrum. Meth. A 672 (2012) 82 Na elastic and

More information

High-precision (p,t) reactions to determine reaction rates of explosive stellar processes Matić, Andrija

High-precision (p,t) reactions to determine reaction rates of explosive stellar processes Matić, Andrija University of Groningen High-precision (p,t) reactions to determine reaction rates of explosive stellar processes Matić, Andrija IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's

More information

Dipole Response of Exotic Nuclei and Symmetry Energy Experiments at the LAND R 3 B Setup

Dipole Response of Exotic Nuclei and Symmetry Energy Experiments at the LAND R 3 B Setup Dipole Response of Exotic Nuclei and Symmetry Energy Experiments at the LAND R 3 B Setup Dominic Rossi for the LAND collaboration GSI Helmholtzzentrum für Schwerionenforschung GmbH D 64291 Darmstadt, Germany

More information

Nuclear Level Density and Gamma Strength from Quasi-Continuum Lifetimes with GRETINA. Leo Kirsch Oslo 5/10/17

Nuclear Level Density and Gamma Strength from Quasi-Continuum Lifetimes with GRETINA. Leo Kirsch Oslo 5/10/17 Nuclear Level Density and Gamma Strength from Quasi-Continuum Lifetimes with GRETINA Leo Kirsch Oslo 5/10/17 Nuclear Level Density and Gamma Strength from Quasi-Continuum Lifetimes with GRETINA 16 MeV

More information

Proton decay and neutrino astrophysics with the future LENA detector

Proton decay and neutrino astrophysics with the future LENA detector Proton decay and neutrino astrophysics with the future LENA detector Teresa Marrodán Undagoitia tmarroda@ph.tum.de Institut E15 Physik-Department Technische Universität München Paris, 11.09.08 Outline

More information

Björn Lehnert. Search for double beta decays of palladium isotopes into excited states

Björn Lehnert. Search for double beta decays of palladium isotopes into excited states Search for double beta decays of palladium isotopes into excited states INTERNATIONAL SCHOOL OF NUCLEAR PHYSICS 35th Course Erice 23/09/2013 Björn Lehnert Institut für Kern- und Teilchenphysik Outline

More information

Primer: Nuclear reactions in Stellar Burning

Primer: Nuclear reactions in Stellar Burning Primer: Nuclear reactions in Stellar Burning Michael Wiescher University of Notre Dame The difficulty with low temperature reaction rates CNO reactions in massive main sequence stars He burning reactions

More information

Latest results from LUNA

Latest results from LUNA Journal of Physics: Conference Series PAPER OPEN ACCESS Latest results from LUNA To cite this article: Rosanna Depalo and LUNA collaboration 2018 J. Phys.: Conf. Ser. 940 012026 View the article online

More information

Universe Cluster and MLL Tandem

Universe Cluster and MLL Tandem Universe Cluster and MLL Tandem Universe Cluster and MLL Tandem Universe Cluster and MLL Tandem Closed since 9 march 2015 Finances for refurbishment granted TUM: 300 k LMU: 200 k UniBW: 100 k Planning:

More information

13 Synthesis of heavier elements. introduc)on to Astrophysics, C. Bertulani, Texas A&M-Commerce 1

13 Synthesis of heavier elements. introduc)on to Astrophysics, C. Bertulani, Texas A&M-Commerce 1 13 Synthesis of heavier elements introduc)on to Astrophysics, C. Bertulani, Texas A&M-Commerce 1 The triple α Reaction When hydrogen fusion ends, the core of a star collapses and the temperature can reach

More information

Measuring Neutron Capture Cross Sections on s-process Radioactive Nuclei

Measuring Neutron Capture Cross Sections on s-process Radioactive Nuclei Measuring Neutron Capture Cross Sections on s-process Radioactive Nuclei 5th Workshop on Nuclear Level Density and Gamma Strength Oslo, May 18-22, 2015 LLNL-PRES-670315 LLNL-PRES-XXXXXX This work was performed

More information

Resonance scattering and α- transfer reactions for nuclear astrophysics.

Resonance scattering and α- transfer reactions for nuclear astrophysics. Resonance scattering and α- transfer reactions for nuclear astrophysics. Grigory Rogachev Outline Studying resonances using resonance scattering Studying resonances using transfer reactions Resonances

More information

Two-Proton Decay Experiments

Two-Proton Decay Experiments Two-Proton Decay Experiments Robert Charity Washington University, St. Louis, USA Classification of 2p decays Goldansky (190) 2p decay (like double β decay) Intermediate state not accessible to 1p decay.

More information

First Results from GRIFFIN Half-lives of Neutron Rich Cd and 131 In! Ryan Dunlop Physics Dept. University of Guelph, Canada INPC 2016

First Results from GRIFFIN Half-lives of Neutron Rich Cd and 131 In! Ryan Dunlop Physics Dept. University of Guelph, Canada INPC 2016 First Results from GRIFFIN Half-lives of Neutron Rich 128-130 Cd and 131 In! Ryan Dunlop Physics Dept. University of Guelph, Canada INPC 2016 r-process High n density! fast capturing! x! Produces many

More information

The 22 Ne(α,n) 25 Mg reaction at astrophysical energies studied via the Trojan Horse Method applied to the 2 H( 25 Mg, α 22 Ne) 1 H reaction

The 22 Ne(α,n) 25 Mg reaction at astrophysical energies studied via the Trojan Horse Method applied to the 2 H( 25 Mg, α 22 Ne) 1 H reaction The 22 Ne(α,n) 25 Mg reaction at astrophysical energies studied via the Trojan Horse Method applied to the 2 H( 25 Mg, α 22 Ne) 1 H reaction R. Spartà 1, M. La Cognata 1, C. Spitaleri 1,2, S. Cherubini

More information

Positron Annihilation Spectroscopy

Positron Annihilation Spectroscopy Positron Annihilation Spectroscopy (1) Angular Correlation θ N x, y = p x, y m C θ γ-ray (511keV ± E) 0 (2) Doppler Broadening Cp E = z 2 θ N p ~100µm 22 Na (e + Source) e - e + ~ 10-12 s Sample γ-ray

More information

Assignment 5. Ian Rittersdorf Nuclear Engineering & Radiological Sciences

Assignment 5. Ian Rittersdorf Nuclear Engineering & Radiological Sciences Assignment 5 Ian Rittersdorf Nuclear Engineering & Radiological Sciences ianrit@umich.edu March 19, 2007 1 All mass values taken from Krane unless otherwise noted. P5.1, 20% Krane, Problem 9.3, p. 332.

More information

Production and Separation of Radioactive Beams. Mg and 20 Na with MARS

Production and Separation of Radioactive Beams. Mg and 20 Na with MARS Production and Separation of Radioactive Beams 20 Mg and 20 Na with MARS Gopal Subedi, Colby College REU 2009, Cyclotron Institute, TAMU Advisor: Dr. Robert E. Tribble August 23, 2009 1 Overview Motivation

More information

Investigation of Pygmy Dipole Resonance in neutron rich exotic nuclei

Investigation of Pygmy Dipole Resonance in neutron rich exotic nuclei Investigation of Pygmy Dipole Resonance in neutron rich exotic nuclei R.Avigo 1,2, O.Wieland 1, A.Bracco 1,2, F.Camera 1,2 on behalf of the AGATA and DALI2 collaborations 1 INFN, sezione di Milano 2 Università

More information

Neutron cross sections in stellar nucleosynthesis: study of the key isotope 25 Mg

Neutron cross sections in stellar nucleosynthesis: study of the key isotope 25 Mg Neutron cross sections in stellar nucleosynthesis: study of the key isotope 25 Mg SIF - XCIX Congresso Nazionale, Trieste 26 Settembre 2013 Stellar nucleosynthesis Elements in stars are mainly produced

More information

Experimental Neutron Capture Measurements and Nuclear Theory Needs

Experimental Neutron Capture Measurements and Nuclear Theory Needs Experimental Neutron Capture Measurements and Nuclear Theory Needs A. Couture INT 17-1a Univ. of Washington Seattle, WA Slide 1 Outline Why do we need neutron capture Traditional (n,g) measurements Determining

More information

Nuclear Waiting Points and Double Peaked X-Ray Bursts

Nuclear Waiting Points and Double Peaked X-Ray Bursts Nuclear Waiting Points and Double Peaked X-Ray Bursts WITH TODAY'S HONORARY CO-AUTHORSHIP: David Miles Kahl Department of Physics & Astronomy, McMaster University, 1280 Main Street West, ABB 248, Hamilton,

More information

b delayed g decay measurements to probe thermonuclear astrophysical explosions

b delayed g decay measurements to probe thermonuclear astrophysical explosions b delayed g decay measurements to probe thermonuclear astrophysical explosions Chris Wrede Michigan State University and NSCL for the NSCL E10034, E12028 & E14066 collaborations NIC XIII, Debrecen, Hungary

More information