Indirect techniques for astrophysical reaction rates determinations. Faïrouz Hammache (IPN-Orsay)
|
|
- Jessie Anthony
- 5 years ago
- Views:
Transcription
1 Indirect techniques for astrophysical reaction rates determinations Faïrouz Hammache (IPN-Orsay) Nucleus Nucleus 015 Catania, 1-6 June 015
2 Why indirect techniques? Astrophysics reactions Weak energies : few kev to few MeV E C (E) very weak (fb-pb) (E) (exponential) when E 1 E S E exp( ) E Direct measurements of (E) at high energies then extrapolation at stellar energies Problems with extrapolation: sub-threshold resonances, resonances at very low energy Radioactive nuclei (novae, r or s-process ): low intensities (~10 5 p/s) or targets with few atoms/cm direct measurements difficult or impossible? Subthreshold resonance S(E) E r Extrapolation? Gamow peak low energy direct measurements Low energy tail of large resonances Non resonant capture high energy E cm
3 Ingredients needed to evaluate & N A v Resonant reactions: A+xC*B+y or A+xC*C+ E cm l S A + x J E R p n Resonant reaction J C Resonant capture only possible for energies: E cm =E R =E x -Q E cm B+y v kt R 3 J c R exp kt J A 1 J x 1 tot Resonant reaction rates can be calculated if the resonant parameters (E R, J, i, i / tot,...) are known Indirect techniques & reactions can be used to extract these spectroscopic information: Transfer, THM, Coulomb dissociation, ANC, inelastic scattering, charge exchange reactions 1 E R x y
4 Massive stars & 1 C(,) 16 O reaction Crucial for energetics, nucleosynthesis, final fate of the stars, 1 C(,) 16 O 40% incertainty T=0. GK Gamow peak ~300 kev, (E 0 ) ~ 10-8 nb Direct 300 kev impossible Direct E cm 900 kev Need of precise data at high energies & extrapolation at 300 kev (R-matrix formalism) BUT Overlap of various contributions:? E1 & E transitions to the gs: Effect of the high energy tail of the 1 - & + sub-threshold resonances (S, γ α?) S (1 - ) !? S ( + ) !? & Interference effect & cascades? Study of 6.9 & 7.1 MeV states 16 O via the transfert reaction 1 C( 7 Li,t) 16 O
5 Experimental Set-up Split-Pole spectrometer (Tandem/ALTO) W ~ 1.7 msr E/E ~ 5 x H 3 H target 7 34,8MeV Faraday cup Position gas chamber, 4 + =11, -, 1 -, + Plastic scintillator (E) - d/dw measurements up to 45 E proportional gas counter - Strong population of the cluster + & 4 + state direct transfer mechanism - Population (weak) of the -, 8.87 MeV state compound nucleus? FR-DWBA & HF calculations
6 Results: Comparison exp & calculations r=6.5fm FR- DWBA HF FR-DWBA+HF Good description of the data by DWBA (6.05, 6.13, 6.9, 7.1, 9.58 et MeV) Direct transfer mechanism Disagreement at 10 for the 7.1 MeV Multi-step transfer? d/dw No (CDCC calculations of Keeley) S ( + )= kev S (1 - )= kev ~ C ~ C ( (1 ) ) (.07 ( ) ) fm fm 1 1 In agreement with ANC experiments Brune et al. 001 Avila et al. 014
7 Fit R-matrix calculations E & E1 components phase shifts data 1 C(,) 1 C measurements 1 C(,) 16 O astrophysical S-factors (direct data) γ α of the + & 1 - sub-threshold states are fixed parameters Tischhauser et al. =1.0 Tischhauser et al. =3.5
8 Fit R-matrix calculations E & E1 components phase shifts data 1 C(,) 1 C measurements 1 C(,) 16 O astrophysical S-factors (direct data) γ α of the + & 1 - sub-threshold states are fixed parameters Tischhauser et al. =1.0 Tischhauser et al. =3.5 =3.6 =.3 S E (300 kev)=5019 kev-barn S E1 (300 kev)=1008 kev-barn In excellent agreement with ANC results of Brune et al. 001 (γ α ( + ) & γ α (1 - ) fixed) In agreement with other works (γ α ( + ) & γ α (1 - ) free parameters) within error bars but central values 0% (E1) & 30% (E) N. Oulebsir, F. Hammache et al. PRC 85, (01)
9 WMAP Big-Bang Nucleosynthesis & 7 Li problem Primordial nucleosynthesis (BBN) of light elements is one of the three observational pillars of the Big Bang model together with the expansion of the Universe & the Cosmic Microwave Background radiation Observations He shell When T 10 9 K BBN begins : D, 4 He, 3 He, 7 Li synthesized via nuclear reactions Abundances depend on W B h W B h = (WMAP) (Komatsu et al. 011) (BBN+CMB) predictions (D, 3 He, 4 He) observations But: ( 7 Li/H) BBN / ( 7 Li/H) obs 3!!! (Coc et al. 013) 3 7 Li problem. Metal poor Halo dwarf stars
10 Nuclear solution to 7 Li problem? 7 Li production via EC of 7 Be: 7 Be production: 3 He( 4 He,) 7 Be known better than 8% (Adelberger et al. 010, Di Leva et al. 013) 7 Be destruction: 7 Be(n,p) 7 Li(p,) very well known (Descouvemont et al. 004) Missing 7 Be destruction channels? Chakraborty et al. 011, Civitarese et al (+) 7 Be+d 9 B* MeV (5/ + ) state Angulo et al. 005, O'Malley et al. 011, Scholl et al Be+ 3 He 10 C* hypothetical state at ~ 15 MeV (1 -, - ) 7 Be+ 4 He 11 C* hypothetical state at ~ 7.8 MeV Be+ 3 He Existence? ( -, 1 - ) ( -, 1 - ) ( + ) C states? p? B+p Be+
11 Search for missing 10 C & 11 C states & Experimental Results 10 B( 3 He,t) 10 C & 11 B( 3 He,t) 11 C charge-exchange 35 MeV Tandem-ALTO SP =7,10, B( 3 He,t) 11 C spectrum 10 B( 3 He,t) 10 C spectrum He shell No additional state in 11 C at ~ 7.8 MeV Only statistical fluctuations All known 11 B mirror nucleus states below E x = 9 MeV have their counterpart in 11 C No obvious additional state in 10 C at ~ 15 MeV Contamination peaks due to 16 O Same results at other angles (7º and 15º)
12 10 C state 95% confidence level 7 Be+ 3 He reaction rates & impact on 7 Li Simulation of a state in the region of interest with various tot & d/dw 3 He,t & same target thickness, number of incident 3 He ions & energy resolution as experiment Er= 10-, 100-, 500- kev tot = 590 kev tot = 00 kev He shell exclusion zone Typical ( 3 He,t) cross-sections to 1 -, - 10 d/dw > 5 b/sr If present total 590 kev (95% CL) F. Hammache, A. Coc et al. PRC 88, 0680 (R) 013 3He from Wigner limit ( W = 1.84 MeV) in all cases ( 3 He) << tot tot = p or BBN calculations: no impact on 7 Li 7 Li problem not due to resonant states in 10 C & 11 C
13 10 C state 95% confidence level 7 Be+ 3 He reaction rates & impact on 7 Li Simulation of a state in the region of interest with various tot & d/dw 3 He,t & same target thickness, number of incident 3 He ions & energy resolution as experiment Er= 10-, 100-, 500- kev tot = 590 kev tot = 00 kev He shell exclusion zone Typical ( 3 He,t) cross-sections to 1 -, - 10 d/dw > 5 b/sr If present total 590 kev (95% CL) F. Hammache, A. Coc et al. PRC 88, 0680 (R) 013 3He from Wigner limit ( W = 1.84 MeV) in all cases ( 3 He) << tot tot = p or BBN calculations: no impact on 7 Li 7 Li problem not due to resonant states in 10 C & 11 C
14 6 Al observations & Nucleosynthesis Massive stars: (> 8 M ) Wolf-Rayet phase and ccsne + Observations of 6 Al (T 1/ = y) 6 Al 6 Mg* 6 Mg MeV Credit: MPE Garching / R. Diehl Allende meteorite Source of 6 Al? Astrophysical context of Solar System formation Cameron et al., 1977 Tatischeff et al., Al nucleosynthesis in massive stars: Core H burning Ne/C convective shell burning explosive Ne burning Limongi et al., 006 & Woosley et al., 007, Iliadis et al Al yield depends crucially on 6 Al(n,p) and 6 Al(n,) reactions Rates x 6 Al yield/
15 7 Al levels above neutron threshold 7 Al(p,p') 7 Al* inelastic 18 MeV TANDEM-ALTO SP = 10, 5, 40, 45 Deconvolution above neutron threshold (S n = MeV): energy resolution 14 kev Q lab = 40 Comparison with known levels: Very good agreement with 3 Na(,) 7 Al and 6 Al(n,) 3 Na (de Voigt et al. 1971, de Smet et al. 007, Whitmire et al. 1974) about 30 new resonances above S n! Resonance's spins? (,) and (n,) preferentially populate high-spins (J>7/) new resonances probably have low-spins S. Benamara, N. de Séréville et al. PRC89, (014)
16 S n = MeV 7 Al(p,p ) Q3D (MLL) S n kev E x S n Q3D E/E = x 10-4 W = 14 msr Split-Pole E=18 MeV I = 300 na t= 6h Q3D E=0 MeV I = 1 A t= h Confirmation of SP data with better energy resolution (~7 kev) & precision (~ kev) New states observed
17 Coincidence Orsay Experimental conditions: 3 W-type DSSSDs strips (E ~ 0 kev FWHM) close geometry around the target d ~ 11 cm, e ~ 4% Low background environment Beam intensity ~ 100 na! Coincidence spectrum: 6 Al(n,p) 6 Mg dominated by (n,p 1 ) channel
18 Coincidence Orsay Experimental conditions: 3 W-type DSSSDs strips (E ~ 0 kev FWHM) close geometry around the target d ~ 11 cm, e ~ 4% Low background environment Beam intensity ~ 100 na! Coincidence spectrum: 6 Al(n,p) 6 Mg dominated by (n,p 1 ) channel
19 Collaborators IPN-Orsay: F. Hammache, N. de Séréville, I. Stefan, P. Roussel, S. Ancelin, M. Assié, L. Audouin, D. Beaumel, S. Franchoo, B. Le Crom, L. Lefebvre, I. Matea, A. Matta, G. Mavilla, P. Morfouace, L. Perrot, D. Suzuki, M. Vandebrouck University of Béjaïa: N. Oulebsir University of Tizi-Ouzou: S. Benamara CSNSM-Orsay: A. Coc, C. Hamadache, J. Kiener, A. Lefebvre-Schuhl, V. Tatischeff University of York: P. Adsley, A. Laird, C. Barton, C. Diget, S. Fox, C. Nsangu University Libre de Bruxelles: P. Descouvemont University of Huelva: G. Marquinez Duran, A. M. Sanchez-Benitez GANIL-Caen: F. de Oliveira, P. Ujic UPC Barcelona: A. Parikh ASCR-Rez, Czeh Republic: J. Mzarek
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 informationarxiv:nucl-ex/ v1 2 Aug 2004
1 arxiv:nucl-ex/0408001v1 2 Aug 2004 The 18 F(p,α) 15 O reaction rate for application to nova γ-ray emission N. de Séréville a, E. Berthoumieux b and A. Coc a a CSNSM, CNRS/IN2P3/UPS, Bât. 4, 91405 Orsay
More informationHe-Burning in massive Stars
He-Burning in massive Stars He-burning is ignited on the He and ashes of the preceding hydrogen burning phase! Most important reaction -triple alpha process 3 + 7.6 MeV Red Giant Evolution in HR diagram
More informationnuclear states nuclear stability
nuclear states 1 nuclear stability 2 1 nuclear chart 3 nuclear reactions Important concepts: projectile (A) target (B) residual nuclei (C+D) q-value of a reaction Notations for the reaction B(A,C)D A+B
More informationR-matrix Analysis (I)
R-matrix Analysis (I) GANIL TALENT SchoolTALENT Course 6 Theory for exploring nuclear reaction experiments GANIL 1 st -19 th July Ed Simpson University of Surrey e.simpson@surrey.ac.uk Introduction Why
More informationStellar 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 informationNuclear 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 informationLecture #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 informationin2p , 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 informationThe Application of R-Matrix Analysis to Experimental Data. 1 - Resonance Properties. Alex Murphy & David Mountford
The Application of R-Matrix Analysis to Experimental Data 1 - Resonance Properties Alex Murphy & David Mountford Contents The R-Matrix Formalism Context: The 18 F(p,α) 15 O Reaction (Doing an ) R-Matrix
More informationH/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 informationNew measurement of the cross section of the Big Bang nucleosynthesis reaction D(α,γ) 6 Li and its astrophysical impact
New measurement of the cross section of the Big Bang nucleosynthesis reaction D(α,γ) 6 Li and its astrophysical impact F. Hammache 1,2, D. Galaviz 3, K. Sümmerer 2, S.Typel 2, F. Uhlig 2, A. Coc 4, F.
More informationThe 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 informationReaction rates for nucleosynthesys of light and intermediate-mass isotopes
Reaction rates for nucleosynthesys of light and intermediate-mass isotopes Gianluca Imbriani Physics Department of University of Naples Federico II, Italian National Institute of Nuclear Physics (INFN)
More informationTransfer reactions induced by 56 Ni: pairing and N=28 shell closure
Transfer reactions induced by 56 Ni: pairing and N=28 shell closure Anastasia Georgiadou Supervised by Marlène Assié 20th COLLOQUE GANIL 56Ni: a doubly magic nucleus? N=28 shell closure Experimental set-up
More informationSingle-particle structure of 17 C studied with the 16 C(d,p) transfer reaction
Single-particle structure of 17 C studied with the 16 C(d,p) transfer reaction Franck Delaunay LPC Caen, France XX th Colloque GANIL, 15-20 October 2017 X. Pereira-López 1,2, B. Fernández-Domínguez 2,
More informationPoS(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 informationPrimer: 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 informationNuclear Structure in Astrophysics Recent Examples from the S-DALINAC
TU DARMSTADT 2007 Nuclear Structure in Astrophysics Recent Examples from the S-DALINAC S-DALINAC and research program an overview Selected examples: Deuteron electrodisintegration under 180 and its importance
More informationGALACTIC Al 1.8 MeV GAMMA-RAY SURVEYS WITH INTEGRAL
Proceedings of the 3rd Galileo Xu Guangqi Meeting International Journal of Modern Physics: Conference Series Vol. 23 (2013) 48 53 c World Scientific Publishing Company DOI: 10.1142/S2010194513011069 GALACTIC
More informationResonant 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 informationElectromagnetic and Nuclear Breakup in Coulomb Dissociation Experiments
Electromagnetic and Nuclear Breakup in Coulomb Dissociation Experiments Excellence Cluster Universe, Technische Universität, München GSI Helmholtzzentrum für Schwerionenforschung, Darmstadt S246 Collaboration
More informationExperimental 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 informationthe astrophysical formation of the elements
the astrophysical formation of the elements Rebecca Surman Union College Second Uio-MSU-ORNL-UT School on Topics in Nuclear Physics 3-7 January 2011 the astrophysical formation of the elements lecture
More informationNe(alpha,n) revisited
22 Ne(alpha,n) revisited Joachim Görres University of Notre Dame & JINA Ph.D. Thesis of Rashi Talwar Neutron sources for the s-process Main Component A>100 Weak Component A< 100 low mass AGB stars T= 0.1
More information13 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 informationUpdating Standard Big-Bang Nucleosynthesis after Planck
Updating Standard Big-Bang Nucleosynthesis after Planck Institut d Astrophysique de Paris, CNRS, Université Pierre et Marie Curie, 98 bis Bd Arago, 75014 Paris, France E-mail: vangioni@iap.fr Alain Coc
More informationPerspectives on Nuclear Astrophysics
Perspectives on Nuclear Astrophysics and the role of DUSEL Nuclear Astrophysics is a broad field that needs facilities from 1keV-100GeV A low energy accelerator DIANA a DUSEL is a unique instrument for
More informationIndirect Methods in Nuclear Astrophysics
Indirect Methods in Nuclear Astrophysics 1. Introduction 2. Reaction rates and energy scales 3. Motivation for indirect methods 4. Brief description of some of the methods 5. Nuclear Reaction preliminaries
More informationNuclear Reactions and Astrophysics: a (Mostly) Qualitative Introduction
Nuclear Reactions and Astrophysics: a (Mostly) Qualitative Introduction Barry Davids, TRIUMF Key Concepts Lecture 2013 Introduction To observe the nucleus, we must use radiation with a (de Broglie) wavelength
More informationMeasurement of the neutron spectroscopic factor in 10 Be
Measurement of the neutron spectroscopic factor in 10 Be Ertao Li Shenzhen University, Shenzhen, China Konkoly Observatory, Budapest, Hungary 15 th Mar. 2018 Cooperation: China Institute of Atomic Energy
More informationDetermining 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 informationGamma-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 informationHigh Resolution Spectroscopy in Nuclear Astrophysics. Joachim Görres University of Notre Dame & JINA
High Resolution Spectroscopy in Nuclear Astrophysics Joachim Görres University of Notre Dame & JINA Nuclear Astrophysics Studies at RCNP Osaka Notre Dame Groningen Started in 2002 (Georg @ RCNP) with a
More informationScattering of He on Pb at energies around the Coulomb barrier
Scattering of on Pb at energies around the Coulomb barrier 20 G. Marquínez-Durán1, I. Martel1, K. Rusek2, A.M. Sánchez-Benítez1, L. Acosta3 1 University of Huelva, Spain A. Soltan Institute for Nuclear
More informationNeutron 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 informationResonance 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 informationInteractions. Laws. Evolution
Lecture Origin of the Elements MODEL: Origin of the Elements or Nucleosynthesis Fundamental Particles quarks, gluons, leptons, photons, neutrinos + Basic Forces gravity, electromagnetic, nuclear Interactions
More informationCross section measurements of fusion reactions at astrophysically relevant energies: the LUNA experiment
Cross section measurements of fusion reactions at astrophysically relevant energies: the LUNA experiment Alba Formicola (on behalf of LUNA collaboration) Laboratory Underground Nuclear Astrophysics relative
More informationPreliminary results of the indirect study of the 12 C( 12 C,α) 20 Ne reaction via the THM applied to the 16 O( 12 C,α 20 Ne )α reaction
Preliminary results of the indirect study of the 12 C( 12 C,α) 20 Ne reaction via the THM applied to the 16 O( 12 C,α 20 Ne )α reaction G.G. Rapisarda, 1,2,6 C. Spitaleri, 1,2 C. Bordeanu, 3 Z. Hons, 4
More informationfundamental nuclear physics Get information about the mere nuclear interaction Nuclear tecnologies Nuclear Waste trasmutation Energy production
1 2 fundamental nuclear physics Get information about the mere nuclear interaction NEUTRON INDUCED REACTIONS Nuclear tecnologies Nuclear Waste trasmutation Energy production Nuclear Astrophysics Nucleosynthesis
More informationTopics in Nuclear Astrophysics II. Stellar Reaction Rates
Topics in Nuclear strophysics II Stellar Reaction Rates definition of a reaction rate Gamow window lifetimes of isotopes at stellar conditions nuclear energy production rate introduction to network simulations
More informationHydrogen & Helium Burning in Stars
Hydrogen & Helium Burning in Stars What remains to be done and how to do it! Hydrogen Burning: 4 He, 14 N Helium Burning: 12 C, 16 O, 22 Ne, n, s-nuclei Alba Formicola (on behalf of LUNA collaboration)
More information12 Big Bang Nucleosynthesis. introduc)on to Astrophysics, C. Bertulani, Texas A&M-Commerce 1
12 Big Bang Nucleosynthesis introduc)on to Astrophysics, C. Bertulani, Texas A&M-Commerce 1 12.1 The Early Universe According to the accepted cosmological theories: The Universe has cooled during its expansion
More informationThe Ring Branch. Nuclear Reactions at. Mass- and Lifetime Measurements. off Exotic Nuclei. Internal Targets. Electron and p. Experiments: Scattering
stochastic cooling Exotic nuclei from Super-FRS Degrader for fast slowing down The Ring Branch TOF Detector MCPs E anode ion B CR Electron cooler NESR secondary electrons Experiments: Mass- and Lifetime
More informationCoulomb dissociation of 34 Na and its relevance in nuclear astrophysics
INDIAN INSTITUTE OF TECHNOLOGY ROORKEE Coulomb dissociation of 34 Na and its relevance in nuclear astrophysics Gagandeep Singh Department of Physics, Indian Institute of Technology Roorkee, Roorkee, UK
More informationPrimordial (Big Bang) Nucleosynthesis
Primordial (Big Bang) Nucleosynthesis H Li Be Which elements? He METALS - 1942: Gamow suggests a Big Bang origin of the elements. - 1948: Alpher, Bethe & Gamow: all elements are synthesized minutes after
More informationRadiative-capture reactions
Radiative-capture reactions P. Descouvemont Physique Nucléaire Théorique et Physique Mathématique, CP229, Université Libre de Bruxelles, B1050 Bruxelles - Belgium 1. Introduction, definitions 2. Electromagnetic
More informationWhat Powers the Stars?
What Powers the Stars? In brief, nuclear reactions. But why not chemical burning or gravitational contraction? Bright star Regulus (& Leo dwarf galaxy). Nuclear Energy. Basic Principle: conversion of mass
More informationSemi-Classical perturbation theory Coulomb only First-order most used
direct reactions Models for breakup Semi-Classical perturbation theory Coulomb only First-order most used TDSE (Time Dependent Schrodinger Equation) Coulomb + Nuclear Semi-classical orbit needed DWBA (Distorted
More informationPrimordial Nucleosynthesis
Primordial Nucleosynthesis Alain Coc (Centre de Sciences Nucléaires et de Sciences de la Matière, Orsay) q Standard Big-Bang Nucleosynthesis of 4He, D, 3He, 7Li compared with observations q The SBBN lithium
More informationConstraining 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 informationTHM determination of the 65 kev resonance strength intervening in the 17 O ( p,α) 14 N reaction rate
THM determination of the 65 kev resonance strength intervening in the 17 O ( p,α) 14 N reaction rate M. L. Sergi, C. Spitaleri, S. V. Burjan, S. Cherubini, A. Coc, M. Gulino, F. Hammache, Z. Hons, B. Irgaziev,
More informationNeutron 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 informationCENBG, Bordeaux, France 2. CEA/DAM-DIF, Arpajon,France 3. CEA/DEN, Saint Paul Lez Durance, France 4. IPN Orsay, Orsay France 5
D. Denis-Petit 1, B. Jurado 1, P. Marini 2, R. Pérez-Sanchez 1, M. Aiche 1, S. Czajkowski 1, L. Mathieu 1, I. Tsekhanovich 1,V. Méot 2,O. Roig 2,B. Morillon 2, P. Romain 2, O. Bouland 3, L. Audouin 4,
More informationNucleosynthesis. at MAGIX/MESA. Stefan Lunkenheimer MAGIX Collaboration Meeting 2017
Nucleosynthesis 12 C(α, γ) 16 O at MAGIX/MESA Stefan Lunkenheimer MAGIX Collaboration Meeting 2017 Topics S-Factor Simulation Outlook 2 S-Factor 3 Stages of stellar nucleosynthesis Hydrogen Burning (PPI-III
More informationSolar Fusion Cross Sections for the pp chain and CNO cycles
Solar Fusion Cross Sections for the pp chain and CNO cycles Working Group 10: Theoretical Issues (Wick Haxton, Stefan Typel) status of theory at 1997 meeting (Rev. Mod. Phys. 70 (1998) 1265) progress during
More informationStellar processes, nucleosynthesis OUTLINE
Stellar processes, nucleosynthesis OUTLINE Reading this week: White 313-326 and 421-464 Today 1. Stellar processes 2. Nucleosynthesis Powerpoint credit: Using significant parts of a WHOI ppt 1 Question
More informationSUMMARY. Novae phenomenon see (J.Jose talk) Why is 18 F important? State of knowledge of 18 F(p,a) reaction. What can we learn from the THM study
SUMMARY Novae phenomenon see (J.Jose talk) Why is F important? State of knowledge of F(p,a) reaction What can we learn from the THM study Classical Nova The companion star transfers matter onto the white
More informationarxiv:nucl-ex/ v1 17 Mar 1997
Comparison of low energy resonances in 15 N(α, γ) 19 F and 15 O(α, γ) 19 Ne and related uncertainties F. de Oliveira, A. Coc, P. Aguer, G. Bogaert, J. Kiener, A. Lefebvre, V. Tatischeff, and J.-P. Thibaud
More informationLecture 19 Nuclear Astrophysics. Baryons, Dark Matter, Dark Energy. Experimental Nuclear Physics PHYS 741
Lecture 19 Nuclear Astrophysics Baryons, Dark Matter, Dark Energy Experimental Nuclear Physics PHYS 741 heeger@wisc.edu References and Figures from: - Haxton, Nuclear Astrophysics - Basdevant, Fundamentals
More informationDecay 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 informationNuclear Astrophysics Research at HIγS
Nuclear Astrophysics Research at HIγS Selected Examples of Work in Progress Werner Tornow Duke University & TUNL Outline A. What is HIγS? B. Few-Body Physics (see T. Shima) C. Nuclear Astrophysics 4 9
More informationLecture 4: Nuclear Energy Generation
Lecture 4: Nuclear Energy Generation Literature: Prialnik chapter 4.1 & 4.2!" 1 a) Some properties of atomic nuclei Let: Z = atomic number = # of protons in nucleus A = atomic mass number = # of nucleons
More informationHeavy Element Nucleosynthesis. A summary of the nucleosynthesis of light elements is as follows
Heavy Element Nucleosynthesis A summary of the nucleosynthesis of light elements is as follows 4 He Hydrogen burning 3 He Incomplete PP chain (H burning) 2 H, Li, Be, B Non-thermal processes (spallation)
More informationSURROGATE 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 informationA NEW GENERATION OF GAMMA-RAY TELESCOPE
A NEW GENERATION OF GAMMA-RAY TELESCOPE Aleksandar GOSTOJIĆ CSNSM, Orsay, France 11 th Russbach School on Nuclear Astrophysics, March 2014. Introduction: Gamma-ray instruments GROUND BASED: ENERGY HIGHER
More informationNuclear Astrophysics
Nuclear Astrophysics I. Stellar burning Karlheinz Langanke GSI & TU Darmstadt Aarhus, October 6-10, 2008 Karlheinz Langanke ( GSI & TU Darmstadt) Nuclear Astrophysics Aarhus, October 6-10, 2008 1 / 32
More informationHigh efficiency 3 He neutron detector TETRA for DESIR.
DESIR workshop, May 2010 High efficiency 3 He neutron detector TETRA for DESIR. Yuri Penionzhkevich Joint Institute for Nuclear Research, Dubna Beta Decay of Exotic Nuclei: Goal to study Neutron emission
More information(EXPERIMENTAL) NUCLEAR ASTROPHYSICS. study energy generation processes in stars study nucleosynthesis of the elements
(EXPERIMENTAL) NUCLEAR ASTROPHYSICS Ø Ø study energy generation processes in stars study nucleosynthesis of the elements What is the origin of the elements? How do stars/galaxies form and evolve? What
More informationHigh-resolution Study of Gamow-Teller Transitions
High-resolution Study of Gamow-Teller Transitions Yoshitaka Fujita, Osaka Univ. @CNS-SS, 04.Aug.17-20 Nucleus : 3 active interactions out of 4 Strong, Weak, EM Comparison of Analogous Transitions High
More informationNuclear Astrophysics : an introduction
Nuclear Astrophysics : an introduction Sailajananda Bhattacharya VECC, Kolkata. Astronomy :: a natural science, is the study of celestial objects (i.e., stars, galaxies, planets, moons, asteroids, comets
More informationLecture 15: Nuclear Reactions. RELEVANCE: Basic Research reaction mechanisms structure exotic nuclei
Lecture 15: Nuclear Reactions RELEVANCE: Basic Research reaction mechanisms structure exotic nuclei Applications: analytical tool neutron activation analysis astrophysics origin of elements space radiation
More informationThis paper should be understood as an extended version of a talk given at the
This paper should be understood as an extended version of a talk given at the Abstract: 1 st JINA workshop at Gull Lake, 2002. Recent experimental developments at LANL (Los Alamos, NM, USA) and CERN (Geneva,
More informationCHEM 312: Lecture 9 Part 1 Nuclear Reactions
CHEM 312: Lecture 9 Part 1 Nuclear Reactions Readings: Modern Nuclear Chemistry, Chapter 10; Nuclear and Radiochemistry, Chapter 4 Notation Energetics of Nuclear Reactions Reaction Types and Mechanisms
More informationNuclear Reactions Part III Grigory Rogachev
THE FLORIDA STATE UNIVERSITY National Superconducting Cyclotron Facility Nuclear Reactions Part III Grigory Rogachev Outline Introduction. Resonances in atomic nuclei Role of resonances in era of exotic
More informationNuclear Physics for Astrophysics: from the Laboratory to the Stars
Nuclear Physics for Astrophysics: from the Laboratory to the Stars Livius Trache IFIN-HH Bucuresti-Magurele & Cyclotron Institute, Texas A&M University Texas 2013 Symposium, Dallas, TX, Dec 9-13, 2013
More informationNuclear Binding Energy
5. NUCLEAR REACTIONS (ZG: P5-7 to P5-9, P5-12, 16-1D; CO: 10.3) Binding energy of nucleus with Z protons and N neutrons is: Q(Z, N) = [ZM p + NM n M(Z, N)] c 2. } {{ } mass defect Nuclear Binding Energy
More informationAstrophysics needs and tools: Overview of AZURE
Astrophysics needs and tools: Overview of AZURE Nuclear Cross Sections Analysis and R matrix tools Mini school Ed Simpson University of Surrey May 9 th 10 th 2013 Overview Introduction Why do we need the
More informationLecture 19 Big Bang Nucleosynthesis
Lecture 19 Big Bang Nucleosynthesis As with all course material (including homework, exams), these lecture notes are not be reproduced, redistributed, or sold in any form. The CMB as seen by the WMAP satellite.!2
More informationLewis 2.1, 2.2 and 2.3
Chapter 2(and 3) Cross-Sections TA Lewis 2.1, 2.2 and 2.3 Learning Objectives Understand different types of nuclear reactions Understand cross section behavior for different reactions Understand d resonance
More informationNuclear Reactions. RELEVANCE: Basic Research reaction mechanisms structure exotic nuclei
Nuclear Reactions RELEVANCE: Basic Research reaction mechanisms structure exotic nuclei Applications: analytical tool neutron activation analysis astrophysics origin of elements space radiation effects
More informationA 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 informationInvestigation of the surrogate-reaction method via the simultaneous measurement of gamma-emission and fission probabilities
Investigation of the surrogate-reaction method via the simultaneous measurement of gamma-emission and fission probabilities B. Jurado, P. Marini, M. Aiche, S. Czajkowski, D. Denis-Petit, L. Mathieu, R.
More informationNuclear Reactions with light ion and photon beams; Contributions to Neutrino Astrophysics
Nuclear Reactions with light ion and photon beams; Contributions to Neutrino Astrophysics 1. Incompressibility and Giant Resonances (ISGMR, ISGDR) 2. Charge exchange reactions 3. Photon Beams for (g,g
More informationPresentation 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 informationHigh-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 informationX-RAY BURSTS AND PROTON CAPTURES CLOSE TO THE DRIPLINE. The hydrogen-rich accreted envelopes of neutron stars in binary systems are
1 X-RAY BURSTS AND ROTON CATURES CLOSE TO THE DRILINE T. Rauscher 1, F. Rembges 1, H. Schatz 2, M. Wiescher 3, F.-K. Thielemann 1 The hydrogen-rich accreted envelopes of neutron stars in binary systems
More informationThe 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 informationSubbarrier fusion of carbon isotopes ~ from resonance structure to fusion oscillations ~
Subbarrier fusion of carbon isotopes ~ from resonance structure to fusion oscillations ~ Kouichi Hagino, Tohoku University Neil Rowley, IPN Orsay 1. Introduction: 12 C + 12 C fusion 2. Molecular resonances
More informationMeasurements of the 7 Be+n Big-Bang nucleosynthesis reactions at CRIB by the Trojan Horse method
Measurements of the Be+n Big-Bang nucleosynthesis reactions at CRIB by the Trojan Horse method S. Hayakawa 1, K. Abe 1, O. Beliuskina 1, S. M. Cha 2, K. Y. Chae 2, S. Cherubini 3,4, P. Figuera 3,4, Z.
More informationThe 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 informationThe effect of the enhanced. primordial abundance of 7Li. Chapter 2. 8Li (a, n) 11 B reaction rate on
Chapter 2 The effect of the enhanced 8Li (a, n) 11 B reaction rate on primordial abundance of 7Li One of the essential inputs of the primordial nucleosynthesis calculation is the reaction rates of the
More informationExperimental 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 informationDipartimento di Fisica e Astronomia, Università degli Studi di Catania, Catania, Italy 3
The 17 O(n,α) 14 C neutron induced reaction at the astrophysical energies studied via the Trojan Horse Method G.L. Guardo 1, C. Spitaleri 1,2, V. Burjan 3, S. Cherubini 1,2, S. Chesnevskaya 4, A. Cvetinovic
More informationSpectroscopy of light exotic nuclei using resonance scattering in inverse kinematics.
Spectroscopy of light exotic nuclei using resonance scattering in inverse kinematics. Grigory Rogachev RESOLUT: a new radioactive beam facility at FSU Solenoid 2 Magnetic Spectrograph Magnetic Spectrograph
More informationReaction 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 informationNovae 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 informationLatest 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:Lecture 27: Stellar Nucleosynthesis. Cassieopia A
:Lecture 27: Stellar Nucleosynthesis Cassieopia A Major nuclear burning processes Common feature is release of energy by consumption of nuclear fuel. Rates of energy release vary enormously. Nuclear processes
More information